TRUWIZ 117
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Volume 2016, Issue No.9, Dated: 9 September 2016, 3.00 A.M

September 9, 2016

In Memory of

Late Professor Kotcherlakota Rangadhama Rao

D.Sc. (Madras). D.Sc. (London).

(Birth on 9 September 1899 Early Morning, Berhampur)

Demise on 20 June 1972 at 9h09m at Visakhapatnam,

At his residence, Narasimha Ashram

TRUWIZ-117

Q1. We consider the separate spin evolution of electrons and positrons in electron-positron and electron-positron-ion plasmas. We consider oblique propagating longitudinal waves in this systems. Working in a regime of high density n0 ∼ 1027 cm−3 and high magnetic ﬁeld B0 = 1010 G we report presence of the spin-electron acoustic waves and their dispersion dependencies. In electron-positron plasmas, similarly to the electron-ion plasmas, we ﬁnd one spin-electron acoustic wave (SEAW) at propagation parallel or perpendicular to the external ﬁeld and two spin-electron acoustic waves at the oblique propagation. At the parallel or perpendicular propagation of the longitudinal waves in electron-positron-ion plasmas we found four branches: the Langmuir wave, the positron-acoustic wave and pair of waves having spin nature, they are the SEAW and, as we called it, spin-electron-positron acoustic wave (SEPAW). At the oblique propagation we ﬁnd eight waves: the Langmuir wave, Trivelpiece-Gould wave, pair of positron-acoustic waves, pair of SEAWs, and pair of SEPAWs. Thus, for the ﬁrst time, we report existence of the second positron-acoustic wave existing at the oblique propagation and existence of SEPAWs.

a. Transverse b. Longitudinal c. Oscillatory d. acoustic.

Q2. It is ﬁrmly established by experimental results that neutrinos are almost 100% longitudinally polarized and left-handed. It is also conﬁrmed by neutrino oscillation experiments that neutrinos have tiny but non-zero masses. Since the helicity is not a Lorentz invariant quantity for massive particles, neutrinos cannot be strictly left-handed. On the other hand, it is generally assumed that ultra-relativistic massive fermions can be described well enough by the Weyl equations. We discuss the validity of this assumption and propose a new hypothesis according to which neutrinos can be described by pure helicity states although they are not, [24 Dec 2015 ArXiv]

a. Massless b. massive c. hypothetical d. varied mass.

Q3. Despite the fact that the (Light Sterile Neutrinos) LSν can explain some of the tensions between the current cosmological observations at high- and low-redshift, it seems that a full reconciliation is rather complicated. The main reason is that we do not have a valid explanation to the fact that the LSν is not fully thermalized. With the mixing parameters determined by SBL oscillations, in fact, the LSν should fully thermalize with the active neutrinos. We brieﬂy discuss the main eﬀects of the presence of a Light Sterile Neutrino (LSν) in Cosmology and how its properties can be constrained by Cosmic Microwave Background (CMB) and other measurements such as,

a. Astrophysical b. Astronomy c. Cosmological d. CMB.

Q4. We discuss the possibility that the cold dark matter mass proﬁles contain information on the cosmological constant Λ, and that such information constrains the nature of cold dark matter (CDM). We call this approach Modiﬁed Dark Matter (MDM). In particular, we examine the ability of MDM to explain the observed mass proﬁles of about galaxy clusters. Using general arguments from gravitational thermodynamics, we provide a theoretical justiﬁcation for our MDM mass proﬁle and successfully compare it to the NFW mass proﬁles both on cluster and galactic scales. Our results suggest that indeed the CDM mass proﬁles contain information about the cosmological constant in a non-trivial way. [4 January 2016].

a. 13 b. 15 c. 17 d. 20

Q5. Cosmological models connecting the static Schwarzschild metric with the time dependent Friedmann-Robsertson-Walker (FRW) metric, that generally support only zero-pressure continuity at some interface. Instead of matching two diﬀerent metrics at an interface, Baker proposed the use of the Lemaˆ itre-Tolman metric which can go smoothly from a Schwarzschild-Lemaˆ itre metric near a mass concentration to the Friedmann-Lemaˆ itre metric at large distances and also allows for non-zero pressure. Using a variant of the Bona-Stela condition, we ﬁx a metric and ﬁnd that the geodesic equation contains in its slow-speed limit an eﬀective dark matter (eDM) term. We show that this eDM can explain the eﬀects of the dark matter such as the ﬂatten rotational curve of galaxies, the desirable growth rate for the baryonic matter density perturbation during the matter dominant epoch and the dark matter enhancement on the higher acoustic peaks of the power spectrum of the CMB, [13 Jan 2016]

a. Isotropies b. anisotropies c. dark matter d. geodesic equation.

Q6. Gravity's Rainbow by Joao Maqueijo, Lee Smolin: Non-linear special relativity (or doubly special relativity) is a simple framework for encoding properties of flat quantum space-time. In this paper we show how this formalism may be generalized to incorporate curvature (leading to what might be called “doubly general relativity''). We first propose a dual to non-linear realizations of relativity in momentum space, and show that for such a dual the space-time invariant is an energy-dependent metric. This leads to an energy-dependent connection and curvature, and a modification to Einstein's equations. We then examine solutions to these equations. We find the counterpart to the cosmological metric, and show how cosmologies based upon our theory of gravity may solve the “horizon problem''. We discuss the Schwarzchild solution, examining the conditions for which the horizon is energy dependent. We finally find the weak field limit. [Submitted on 14 May 2003 (v1), last revised 3 Feb 2004 (this version, v2)] Modification to Einstein equations are

a. Random b. selective c. simple d. vibrant.

Q7. We have considered the possibility that a compact star is aﬀected by Gravity’s Rainbow. Since the action of Gravity’s Rainbow is prevalently at Planckian length scales, we ﬁnd that in case of isotropic pressure and constant energy density, a star of Planckian size if it is formed, and satisﬁes the usual Buchdahl-Bondi bound, is also stable. On the other hand, when the variable energy density case is considered and an equation of state is introduced, one ﬁnds that, from the relation pr = ωρ(r), ω becomes a function of E/EPl, necessarily. It is interesting to note that the constant energy density and the Misner- Zapolsky energy density are two particular cases of the Dev-Gleiser potential which is of the form ρ(r) = ρ0 + A r² , where ρ0 is the parameter of the constant energy density case and A = 3c² /(56πG). Note that in both cases, namely the constant and variable energy density case, also the mass becomes a function of E/EPl. Here we have considered the simple case where E/EPl is not dependent on the radius r. Of course, other than introducing an anisotropy, the case in which E/EPl becomes E(r)/EPl will be a subject of a future investigation as well as the full examination of the Dev-Gleiser [January 6, 2016 1:19 WSPC Proceedings - 9.75in x 6.5in MG14RStarsV3 page 66]

a. Potential b. charge c. power d. function

Q8. The Mira variable LX Cyg showed a dramatic increase of its pulsation period in the recent decades and appears to undergo an important transition in its evolution. Aims: We aim at investigating the spectral type evolution of this star over the recent decades as well as during one pulsation cycle in more detail and discuss it in connection with the period evolution. Methods: We present optical, near- and mid-IR low-resolution as well as optical high-resolution spectra to determine the current spectral type. The optical spectrum of LX Cyg has been followed for more than one pulsation cycle. Recent spectra are compared to archival spectra to trace the spectral type evolution and a Spitzer mid-IR spectrum is analysed for the presence of molecular and dust features. Furthermore, the current period is derived from AAVSO data. Results: It is found that the spectral type of LX Cyg changed from S to C sometime between 1975 and 2008. Currently, the spectral type C is stable during a pulsation cycle. It is shown that spectral features typical of C-type stars are present in its spectrum from ~0.5 to 14 μm. An emission feature at 10.7 μm is attributed to SiC grains. The period of LX Cyg has increased from ~460 d to ~580 d within only 20 years, and is stable now. Conclusions: We conclude that the change in spectral type and the increase in pulsation period happened simultaneously and are causally connected. Both a recent thermal pulse (TP) and a simple surface temperature decrease appear unlikely to explain the observations. We therefore suggest that the underlying mechanism is related to a recent third dredge-up mixing event that brought up carbon from the interior of the star, i.e. that a genuine abundance change happened. We propose that LX Cyg is a rare transition type object that is uniquely suited to study the transformation from O- to C-rich, [arXiv:1511.02159 [astro-ph.SR] arxiv.org/abs/1511.02159v2]

a. Voids b. giants c. galaxies d. stars

Q9. Neutrinos are neutrally charged particles that have nearly no mass, making it possible for them to pass though most matter, such as our bodies. Scientists believe they come into existence as part of radioactive decay and have been working on ways to prove their existence physically by capturing them with detectors. At the facility in Italy, researchers have set up a large underground tank filled with 300 metric tons of liquid scintillator, when a neutrino collides with one of its particles, a flash of light is emitted, indicating that a single neutrino has been detected. The team at the site has been monitoring the detector since 2007. In this latest research effort, the team is reporting on what have been named geo-neutrinos, which are neutrinos that come from the Earth, either the crust (many of which are thought to come from man-made nuclear reactors) or the mantle. These particles, the team notes, are actually antimatter versions of neutrinos, and have been recorded before, but the detections were very faint, making it difficult to confirm their source. In this new effort, the team looked at detections occurring over 2056 days, with 5.9 sigma [Team records neutrinos from the Earth's mantle, August 10, 2015 by Bob Yirk].

a. Magnitude b. Value c. significance d. correction

Q10. (Phys.org)—An international team of astronomers led by Behnam Javanmardi of the University of Bonn in Germany has recently discovered 11 low surface brightness (LSB) systems located around nearby spiral galaxies. The researchers used small amateur telescopes to scan the sky around large galaxies and successfully obtained the images of their dim companions. A paper reporting the findings appeared last week on the ArXiv pre-print server. By publishing the latest findings, Javanmardi and his colleagues have demonstrated that a search for LSB objects can be successfully performed with a telescope of small diameter, from 0.1 to 1 meter, having a wide field of view. The DGSAT observations were conducted with a network of privately owned robotic observatories equipped with modest-sized telescopes located in Europe, the United States, Australia and Chile. [Astronomers discover low surface brightness …………….. with amateur telescopes, [November 18, 2015 by Tomasz Nowakowski]. Fill the blank,

a. Galaxies b. Quasars c. planets d. stars.

Q11. A topological insulator is a material with non-trivial topological order that behaves as an insulator in its interior but whose surface contains conducting states, meaning that electrons can only move along the surface of the material. However, the conducting surface is not the unique character of topological insulator, since the ordinary band insulators can also support conductive surface states. What is special is that the surface states of topological insulators are symmetry projected by particle number conservation and time reversal symmetry. The spin-momentum locking in the topological insulator allows symmetry protected surface states to host Majorana Particles if superconductivity is induced on the surface of 3D topological insulators via proximity effects (Note that Majorana zero-mode can also appear without topological insulators) The non-trivialness of topological insulators is encoded in the existence of a gas of helical Dirac fermions. Helical Dirac Fermions, which behave like massless relativistic particles, have been observed in 3D topological insulators. Note that the gapless surface states of topological insulator differ from those in the Quantum Hall Effect, the gapless surface states of topological insulator are symmetry protected (i.e. not topological), while the gapless surface states in Quantum Hall Effect are topological (i.e. robust against any local perturbations that can break all the symmetries). The Z₂ topological invariants cannot be measured using traditional transport methods, such as spin Hall conductance, and the transport is not quantized by the Z₂ invariants. An experimental method to measure Z₂ topological invariants was demonstrated which provide a measure of the Z₂ topological order. Hsieh, D.; D. Hsieh, Y. Xia, L. Wray, D. Qian, A. Pal, J. H. Dil, F. Meier, J. Osterwalder, C. L. Kane, G. Bihlmayer, Y. S. Hor, R. J. Cava and M. Z. Hasan (2009). "Observation of Unconventional Quantum Spin Textures in Topological Insulators". Science 323 (5916): 919–922. Bibcode: 2009, 919H. doi:10.1126/science.1167733. (Note that the term Z₂ topological order has also been used to describe the topological order discovered theory in 1991, with emergent Z₂.)

a. Field b. Theory c. gauge d. potential

Q12. A Galactic Graviton of 5D (dimensional) (2, 1, 0, -1, -2) interacts with a Dark Entity in space-time environment with most of its energy lost to the Dark Entity. Fractional 5D-Meson (1, 1, 0, -1, -1) and a 5D-photon (1, 0, 0, 0, -1) are produced that survive in space-time environment for a minimal time of their existence. 5D-Meson soon disintegrates into an ordinary π–Meson (1, 0, -1) and ordinary photon (1, -1). The 5D-photon out of the Dark Entity disintegrates into ordinary photon (1, -1) and to a set of three Dark Scalars (0, 0, 0). An Anti-Photon released from the Earth interacts with the π–Meson releasing a μ–Meson and an anti-neutrino. The π–Meson is the result of production from distant galaxies gravitational interaction with Dark Entities. This is a new finding. The idea is that the DARK SCALAR traverses with the velocity of light, literally, with the accompanied Mu particle and its neutrino. While the Mu along with its neutrino, travels with a velocity almost near the velocity of light but not equal to it. This saves in the present theory that the LORENTZ’S CONTRACTION concept is indeed preserved (or else the time dilation concept held) but only for the µ particle and its associate neutrino. The DARK SCALAR literally holds the assembly of the µ particle and its neutrino but specifically for a limited period of time, when eventually its’ (the µ particle and its neutrino) interaction with the Earth’s interior matter releases it. Of course, the different lengths and time durations of the µ particle and its neutrino, during their travel, with differing magnitudes, certainly asserts, the possibility of DARK SCALARS of varied types are involved. This accounts for all the different three …………. envisioned in the present theory and formulation. [Presented Paper No.15, Mathematics Department, Mysure University, on 5 Jan 2016, between 3 to 6 PM]

a. Scalars b. Vectors c. Spins d. Magnitudes

Q13. Anti-fractional integral formalism to bring out New Physics for the Spin ±1/8 to ±31/8 in steps of ±1/8^th devoid of integrals. ABSTRACT: An object of my work is that the Anti-Photon [Ref. Physics Section ISCA 2015, held at Mumbai Univ., Jan 5^th] series presents the possibility of higher fractional spins, the formalism and data presented in this paper on Anti-fractional integral formalism specifically brings out the new mathematics for the spin ±1/8 to spin ±31/8 entities. The formalism extension to higher spins is also worked out. [Presented Paper No. Physics Department, Mysure University, on 5 Jan 2016, between 3 to 6 PM].

a. Sizes b. Entities c. Quantities d. Values

Q14. A remote galaxy shining with the light of more than 300 trillion suns has been discovered using data from NASA's Wide-field Infrared Survey Explorer (WISE). The galaxy is the most luminous galaxy found to date and belongs to a new class of objects recently discovered by WISE, extremely luminous infrared galaxies, or ELIRGs. The brilliant galaxy, known as WISE J224607.57-052635.0, may have a behemoth black hole at its belly, gorging itself on gas. Supermassive black holes draw gas and matter into a disk around them, heating the disk to roaring temperatures of millions of degrees and blasting out high-energy, visible, ultraviolet, and X-ray light. The light is blocked by surrounding cocoons of dust. As the dust heats up, it radiates

a. UV light b. Hot Waves c. X-Rays d. Infra-Red light.

Q15. May 25, 2015: (Phys.org): A team of researchers working in Japan has demonstrated that it is possible to conduct a spin current through a short segment of germanium at room temperature. In their paper published in the journal Physical Review Letters, the team describes their technique which could help lead to the development of spintronic devices. To find out, if it might work also at room temperature, the researchers doped a layer of germanium with phosphorous (to serve as an electron donor) which grew on a silicon substrate. A spin current was injected (using microwaves) into the germanium via a ferromagnetic strip (which caused the spins to be aligned) placed on one side of the germanium layer. The current moved through the material towards a strip made of metal on the other side of the germanium layer, where it was subsequently detected by a device able to note spin polarization. The team reports that the current moved successfully through the strip, which was 660 nanometres thick, a distance comparable to other materials that are being tested and which is actually larger than the distance between size features in integrated circuits. That means a circuit could conceivably be made with information passing between two or more spintronic

a. Items b. couples c. devices d. slots

Q16. March 30, 2015: Our main result is that outside a small region near a binary star, [either rocky or gas-giant] planet formation can proceed in much the same was as around a single star," they write. "In our scenario, planets are as prevalent around binaries as around single stars." In their study, Bromley and Kenyon showed mathematically and by simple computer simulations that rocky, Earth-sized planets can form around binary stars if they have the oval "most circular" orbit. They didn't conduct their simulations to the point of planet formation, but showed that planetesimals could survive without collisions for tens of thousands of years in concentric, oval-shaped orbits around binary stars. Kepler has found seven planets orbiting within or near the habitable zone around binary stars, but all of them are giant gaseous,

a. Planets b. Stars c. Dwarfs d. Moons

Q17. To directly measure the change in a gradient, the team used measurements made at three different heights. Measuring gravity at two locations close to one another can give the gradient as the measured difference of the two divided by the distance between them. Measuring gravity at three locations allows for calculating the rate of change, or curvature, an idea for an experiment to carry out this measurement was first proposed back in 2002. The experiment conducted by the team in Italy is based on that proposal. To allow for measuring gravity at three locations all at the same time, the team created three plumes of ultra-cold atoms at three different heights inside of a one meter pipe. The top half of the piper was surrounded by tungsten alloy weights to cause an increase in variation of the gravitational field. The atoms were irradiated with pulses from a laser to cause them to separate the plumes into two parts, one that absorbed photons and a second that was left in a ground state. The additional momentum caused the atoms in the first group to fall a different distance over a measured time period, which led to a difference in quantum wave cycles that elapsed between the two. The team then added two more wave pulses to cause the two groups to recombine, which allowed them to interfere. Measuring the interference allowed for calculating the variations in gravitational acceleration and curvature, which turned out to be 1.4×10 ⁻⁵ s ⁻² m ⁻¹, as predicted. [Phys. Rev. Lett. 114, 013001 – Published 5 January 2015.]

a. 1.4E-05 s⁻² m⁻¹ b. 1.4E-06 s⁻² m⁻¹ c.1.5E-06 s⁻² m⁻¹ d 1.5E-06 s⁻² m⁻¹ .

Q18. April 6, 2015 (Phys.org): A team of researchers with the University of Adelaide and the Australia, National University has found that the excited state of the Lambda baryon, Λ (1405), is actually a type of quark molecule. In their paper published in the journal Physical Review Letters, the researchers describe how they ran simulations on a computer that confirmed the properties of the unique particles. One such particle Λ (1405) has been the focus of much research and discussion among physicists as it has defied the description of a typical baryon (a subatomic particle with a mass greater than or equal to a proton and which exist as a nucleon or hyperon) they are supposed to have three quarks. Instead, they have shown behaviour that suggests a molecule-like structure consisting of a quark pair and a triplet, prior research has shown that it takes less energy to cause it to be excited than should be the case for three quarks bound together, suggesting that there is something else at play, such as extra quarks. Some researchers in the past had theorized that Λ (1405) particles could be actually be a combination of mesons and baryons which would result in a particle "molecule" with five quarks.

a. Three quarks b. Four Quarks c. Five Quarks d.one Quark

Q19. May 30, 2014: Back in 1974, space scientists discovered Sagittarius A* (SgrA ∗), a bright source of radio waves emanating from what appeared to be near the centre of the Milky Way galaxy. Subsequent study of the object led scientists to believe that it was (and is) a black hole—the behaviour of stars nearby, for example, suggested it was something massive and extremely dense. What we're able to see when we look at SgrA∗ are plasma gasses near the event horizon, not the object itself as light cannot escape. That should be true for wormholes too, of course, which have also been theorized to exist by the Theory of General Relativity. Einstein even noted the possibility of their existence. Unfortunately, no one has ever come close to proving the existence of wormholes, which are believed to be channels between different parts of the universe, or even between two universes in multi-universe theories. In their paper, Li and Bambi suggest that there is compelling evidence suggesting that many of the objects we believe to be black holes at the centre of galaxies, may in fact be wormholes. Plasma gases orbiting a black hole versus a wormhole should look different to us, the pair suggest, because wormholes should be a lot smaller. Plus, the presence of wormholes would help explain how it is that even new galaxies have what are now believed to be black holes, such large black holes would presumably take a long time to become so large, so how can they exist in a new galaxy? They can't Li and Bambi conclude, instead those objects are actually wormholes, which theory suggests could spring up in an instant, and would have, following the

a. Black Hole b. Big bang c. hot wholes d. Neutron Stars

Q20. Orbital optical lattices with bosons: T. Kock1, C. Hippler1, A. Ewerbeck1, and A. Hemmerich (Dated: January 5, 2016): This article provides a synopsis of our recent experimental work exploring Bose-Einstein condensation in metastable higher Bloch bands of optical lattices. Bipartite lattice geometries have allowed us to implement appropriate band structures, which meet three basic requirements: the existence of metastable excited states suﬃciently protected from collisional band relaxation, a mechanism to excite the atoms initially prepared in the lowest band with moderate entropy increase, and the possibility of cross-dimensional tunnelling dynamics, necessary to establish coherence along all lattice axes. A variety of bands can be selectively populated and a subsequent thermalisation process leads to the formation of a condensate in the lowest energy state of the chosen band. As examples the 2nd, 4th and 7th bands in a bipartite square lattice are discussed. In the 2nd and 7th band, the band geometry can be tuned such that two inequivalent energetically degenerate energy minima arise at the X±-points at the edge of the 1st Brillouin zone. In this case even a small interaction energy is suﬃcient to lock the phase between the two condensation points such that a complex-valued chiral superﬂuid order parameter can emerge, which breaks time reversal symmetry. In the 4th band a condensate can be formed in the Γ-point in the centre of the 1st Brillouin zone, which can be used to explore topologically protected band touching points. The new techniques to access orbital degrees of freedom in higher bands greatly extend the class of many-body scenarios that can be explored with bosons in optical

a. Modes b. lattices c. thresholds d. zones

Q21. On-Chip Microwave Quantum Hall Circulator: A. C. Mahoney,J. I. Colless,S. J. Pauka,J. M. Hornibrook,D. Watson,G. C. Gardner, M. J. Manfra,A. C. Doherty, and D. J. Reilly, david.reilly@sydney.edu.au: Circulators are non-reciprocal circuit elements integral to technologies including radar systems, microwave communication transceivers, and the readout of quantum information devices. Their non-reciprocity arises from the interference of microwaves over the centimetre-scale of the signal wavelength in the presence of bulky magnetic media that break time-reversal symmetry. Here we realize a completely passive on-chip microwave circulator with size 1/1000th the wavelength by exploiting the chiral, ‘slow-light’ response of a 2-dimensional electron gas (2DEG) in the quantum Hall regime. For an integrated GaAs device with 330 µm diameter and ∼ 1 GHz centre frequency, a non-reciprocity of 25 dB is observed over a 50 MHz bandwidth. Furthermore, the direction of circulation can be selected dynamically by varying the magnetic ﬁeld, an aspect that may enable reconﬁgurable passive routing of microwave signals on-chip.

a. On-chip b. out-chip c. out of turn d. in turn

Q22. Spin Mechanics, Joseph E. Losby and Mark R. Freeman: 4 Jan 2016.

The magnetism sub-discipline of spin mechanics is at an exciting stage. Direct experimental insights on the behaviour of spin-rotation coupling in a wide variety of materials is key to a fuller basic understanding of magnetism. Resonant detection of spin angular momentum opens the door to physics not yet explored, such as the timescales associated with the Richardson/Einstein-de Haas eﬀect. The coherent coupling of spin and motion potentially leads to mechanical control of magnetism for applications. Numerous other beneﬁts of spin mechanics will be powerful new mechanical tools for the experimental magnetician’s kit, complementary to existing methods, including fully broadband opto-mechanical labs-on-a-chip for analysis (magnetometry and resonance spectroscopy) of structures from magnetic nano-devices to nanoparticles. [The fourth international workshop on Spin Mechanics will be held on February 20-25, 2017 in Lake Louise, Alberta.]

a. Mesoparticles b. nanoparticles c. pseudo-particles d. spinons

Q23. A small shoulder of optical absorption in polycrystalline HfO2 by LDA+U approach by Jinping Li, Songhe Meng, Liyuan Qin, Hantao Lu, and Takami Tohyama: The dielectric function of the wide-gap optical material HfO2 is investigated by the local density approximation (LDA) +U approach. We focus on the origin of the shoulder-like structure near the edge of the band gap in the imaginary part of the dielectric function, which has been observed on the thin films of monoclinic HfO2. A comparison study on the three polymorphs of hafnia shows that regardless of the underlying crystal structure, the existence of the shoulder is directly controlled by the value of the shortest length of Hf-O bonds. The proposition is further supported by the numerical simulations of isostatic pressing. A possible implication in measurements is suggested accordingly at

a. Low pressure b. high pressure c. medium pressure d. variable pressure.

Q24. Two-dimensional excitonic quasiparticles in a three-dimensional crystal: The case of anatase TiO2: Edoardo Baldini: 6 Jan 2016: Bound electronic excitations play a major role in the electrodynamics of insulators and are typically described by the concept of Wannier-Mott and Frenkel excitons. The former represent hydrogenic electron-hole pairs delocalized over several unit cells of a crystal and they occur in materials with high dielectric constant; the latter correspond to a correlated electron-hole pair localized on a single lattice site and they mostly prevail in molecular solids. Between these two extremes, an intermediate type of excitons exists, typically referred to as charge-transfer excitons. A prototypical system in which these rare quasiparticles have been theoretically predicted but never experimentally conﬁrmed is the anatase polymorph of TiO2, which is one of the most promising material for light-energy conversion applications. Here, we combine angle-resolved photoemission and optical spectroscopies, along with ab initio state-of-the-art theoretical calculations, to demonstrate that the direct optical gap of anatase TiO2 is dominated by a chargetransfer exciton band rising over the continuum of indirect interband transitions. In particular, we ﬁnd that the lowest exciton possesses a two-dimensional nature and is characterized by a giant binding energy of ∼ 300 meV. The universality of these ﬁndings is proven in highly defective samples used in light-energy conversion applications, by interrogating these systems out-of-equilibrium via ultrafast two-dimensional spectroscopy of

a. Narayana b. Rangadhama c. UV d. Infra-Red

Q25. Experimental determination of the massive Dirac fermion model parameters for MoS2, MoSe2, WS2, and WSe2: by Beom Seo Kim, Jun-Won Rhim, Beomyoung Kim, Changyoung Kim, and Seung Ryong Park. 7 Jan 2016. Monolayer MX2 (M = Mo, W; X = S, Se) has drawn much attention recently for its possible application possibilities for optoelectronics, spintronics, and valleytronics. Its exotic optical and electronic properties include a direct band gap, circular polarization dependent optical transitions, and valence band (VB) spin band splitting at the K and −K points. These properties can be described within a minimal model, called the massive Dirac fermion model for which the parameters need to be experimentally determined. We propose that the parameters can be obtained from angle resolved photoemission (ARPES) data from bulk 2H-MX2, instead of monolayer MX2. Through tight binding calculations, we show how the electronic structure at high symmetry points evolves as the system changes from the monolayer to the three dimensional bulk 2H-MX2. We ﬁnd vanishing kz dispersion and almost no change in the direct band gap at the K and −K points, in sharp contrast to the strong kz dispersion at the Γ point. These facts allow us to extract the gap and spin band splitting at the K point as well as the hopping energy from bulk ARPES data. We performed ARPES experiments on single crystals of MoS2, MoSe2, WS2, and WSe2 at various photon energies and also with potassium evaporation. From the data, we determined the parameters for monolayer MoS2, MoSe2, WS2, and WSe2 with the massive fermion model of

a. Einstein b. Boson c. Shahion d Dirac.

Q26. arXiv:1601.02062: Field-induced resistivity plateau and unsaturated negative magnetoresistance in topological semimetal TaSb2: Authors: Yuke Li, Lin Li, Jialu Wang, Tingting Wang, Xiaofeng Xu, Chuanying Xi, Chao Cao, Jianhui Dai: (Submitted on 9 Jan 2016) Abstract: Several prominent transport properties have been identified as key signatures of topological materials. One is the resistivity plateau at low temperatures as observed in several topological insulators (TIs), another is the negative magnetoresistance (MR) when the applied magnetic field is parallel to the current direction as observed in several topological semimetals (TSMs) including Dirac semimetals (DSMs) and Weyl semimetals (WSMs). Usually, these two exotic phenomena emerge in distinct materials with or without time reversal symmetry (TRS), respectively. Here we report the discovery of a new member in TSMs, TaSb2, which clearly exhibits both of these phenomena in a single material. This compound crystallizes in a base-centered monoclinic, centrosymmetric structure, and is metallic with a low carrier density in the zero field. While applying magnetic field it exhibits insulating behavior before appearance of a resistivity plateau below Tc =13 K. In the plateau regime, the ultrahigh carrier mobility and extreme magnetoresistance (XMR) for the field perpendicular to the current are observed as in DSMs and WSMs, in addition to a quantum oscillation behavior with non-trivial Berry phases. In contrast to the most known DSMs and WSMs, the negative MR in TaSb2 does not saturate up to 9 T, which, together with the almost linear Hall resistivity, manifests itself an electron-hole non-compensated TMS. These findings indicate that the resistivity plateau could be a generic feature of topology-protected metallic states even in the absence of TRS and compatible with the negative MR depending on the field direction. Our experiment extends a materials basis represented by TaSb2 as a new platform for future theoretical investigations and device applications of materials,

a. Optical b. Magnetic c. topological d. Sinusoidal

Q27. Resistivity plateau and extremely large magnetoresistance in NbAs2 and TaAs2: Yi-Yan Wang, Qiao-He Yu, and Tian-Long Xia (Dated: January 19, 2016): In topological insulators (TIs), metallic surface conductance saturates the insulating bulk resistance with decreasing temperature, resulting in resistivity plateau at low temperatures as a transport signature originating from metallic surface modes protected by time reversal symmetry (TRS). Such characteristic has been found in several materials including Bi2Te2Se, SmB6 etc. Recently, similar behaviour has been observed in metallic compound LaSb, accompanying an extremely large magetoresistance (XMR). Shubnikov-de Hass (SdH) oscillation at low temperatures further conﬁrms the metallic behavior of plateau region under magnetic ﬁelds. LaSb has been proposed by the authors as a possible topological semimetal (TSM), while negative magnetoresistance is absent at this moment. Here, high quality single crystals of NbAs2/TaAs2 with inversion symmetry have been grown and the resistivity under magnetic ﬁeld is systematically investigated. Both of them exhibit metallic behaviour under zero magnetic ﬁeld, and a metal-to-insulator transition occurs when a nonzero magnetic ﬁeld is applied, resulting in XMR (1.0×105% for NbAs2 and 7.3×105% for TaAs2 at 2.5 K & 14 T). With temperature decreased, a resistivity plateau emerges after the insulator-like regime and SdH oscillation has also been observed in NbAs2 and TaAs2 described as

a. Sda b. SdH c.Sdh d. SdC

Q28. arXiv:1601.04933: Collective magnetic response of CeO2 nanoparticles: Authors: J. M. D. Coey, Karl Ackland, M. Venkatesan, S. Sen: (Submitted on 19 Jan 2016): Abstract: The magnetism of nanoparticles and thin films of wide-bandgap oxides that include no magnetic cations is an unsolved puzzle. Progress has been hampered both by the irreproducibility of much of the experimental data, and the lack of any generally-accepted theoretical explanation. The characteristic signature is a virtually anhysteretic, temperature-independent magnetization curve which saturates in an applied field that is several orders of magnitude greater than the magnetization. It appears as if a tiny volume fraction, < 0.1%, of the samples is magnetic and that the energy scale of the problem is unusually high for spin magnetism. Here we investigate the effect of dispersing 4 nm CeO2 nanoparticles with powders of gamma-Al2O3, sugar or latex microspheres. The saturation magnetization, Ms ~ 60 A/m for compact samples, is maximized by 1 wt% lanthanum doping. Dispersing the CeO2 nanopowder reduces its magnetic moment by up to an order of magnitude. There is a characteristic length scale of order 100 nm for the magnetism to appear in CeO2 nanoparticle clusters. The phenomenon is explained in terms of a giant orbital paramagnetism that appears in coherent mesoscopic domains due to resonant interaction with zero-point fluctuations of the vacuum electromagnetic field. The theory explains the observed temperature-independent magnetization curve and its doping and dispersion dependence, based on a length scale of 300 nm that corresponds to the wavelength of a maximum in the UV absorption spectrum of the magnetic CeO2 nanoparticles. The coherent domains occupy roughly ten percent of the sample volume.

a. Space b. Energy c. absorption d. Volume

Q29. arXiv:1601.04948:Giant semiclassical magnetoresistance in high mobility TaAs2 semimetal: Authors: Desheng Wu, Jian Liao, Wei Yi, Xia Wang, Peigang Li, Hongming Weng, Youguo Shi, Yongqing Li, Jianlin Luo, Xi Dai, Zhong Fang: (Submitted on 19 Jan 2016): Abstract: We report the observation of colossal positive magnetoresistance (MR) in single crystalline, high mobility TaAs2 semimetal. The excellent fit of MR by a single quadratic function of the magnetic field B over a wide temperature range (T = 2-300 K) suggests the semiclassical nature of the MR. The measurements of Hall effect and Shubnikov-de Haas oscillations, as well as band structure calculations suggest that the giant MR originates from the nearly perfectly compensated electrons and holes in TaAs2. The quadratic MR can even exceed 1,200,000% at B = 9 T and T = 2 K, which is one of the largest values among those of all known semi-metallic compounds including the very recently discovered WTe2 and NbSb2. The giant positive magnetoresistance in TaAs2, which not only has a fundamentally different origin from the negative colossal MR observed in magnetic systems, but also provides a nice complemental system that will be beneficial for applications in magneto-electronic devices

a. devices b. systems c. bands d. quadratics

Q30. arXiv:1512.06867: Monolayer MoS2/GaAs heterostructure self-driven photodetector with extremely high detectivity: Authors: Zhijuan Xu, Shisheng Lin, Xiaoqiang Li, Shengjiao Zhang, Zhiqian Wu, Wenli Xu, Yanghua Lu, Sen Xu: (Submitted on 16 Dec 2015): Abstract: Two dimensional material/semiconductor heterostructures offer alternative platforms for optoelectronic devices other than conventional Schottky and p-n junction devices. Herein, we use MoS2/GaAs heterojunction as a self-driven photodetector with wide response band width from ultraviolet to visible light, which exhibits high sensitivity to the incident light of 650 nm with responsivity as 446 mA/W and detectivity as 5.9E13 Jones (Jones = cm Hz^1/2 W^-1), respectively. Employing interface design by inserting h-BN and photo-induced doping by covering Si quantum dots on the device, the responsivity is increased to 582 mA/W for incident light of 650 nm. Distinctly, attributing to the low dark current of the MoS2/h-BN/GaAs sandwich structure based on the self-driven operation condition, the detectivity shows extremely high value of 3.2E14 Jones for incident light of 650 nm, which is higher than all the reported values of the MoS2 based photodetectors. Further investigations reveal that the MoS2/GaAs based photodetectors have high response speed with the typical rise/fall time as 17/31 us. The photodetectors are stable while sealed with polymethylmethacrylate after storage in air for one month. These results imply that monolayer MoS2/GaAs heterojunction may have great potential for practical applications as high performance self-driven photodetectors.

a. Photo-devices b. photo-parts c. photodetectors d. photo-regulators.

Q31.arXiv:1512.02552: Quantum Physics: General spin and pseudospin symmetries of the Dirac equation: Authors: P. Alberto, M. Malheiro, T. Frederico, A. de Castro (Submitted on 8 Dec 2015) Abstract: In the 70's Smith and Tassie, and Bell and Ruegg independently found SU(2) symmetries of the Dirac equation with scalar and vector potentials. These symmetries, known as pseudospin and spin symmetries, have been extensively researched and applied to several physical systems. Twenty years after, in 1997, the pseudospin symmetry has been revealed by Ginocchio as a relativistic symmetry of the atomic nuclei when it is described by relativistic mean field hadronic models. The main feature of these symmetries is the suppression of the spin-orbit coupling either in the upper or lower components of the Dirac spinor, thereby turning the respective second-order equations into Schrodinger-like equations, i.e, without a matrix structure. In this paper we propose a generalization of these SU(2) symmetries for potentials in the Dirac equation with several Lorentz structures, which also allow for the suppression of the matrix structure of second-order equation of either the upper or lower components of the Dirac spinor. We derive the general properties of those potentials and list some possible candidates, which include the usual spin-pseudospin potentials, and also 2- and 1-dimensional potentials. An application for a particular physical system in two dimensions, graphene is suggested with

a. spins b. positrons c. neutrons d. electrons

Q32.arXiv:1512.00288: Emergence of integer quantum Hall effect from chaos: Authors: Chushun Tian, Yu Chen, Jiao Wang: (Submitted on 1 Dec 2015) Abstract: We present an analytic microscopic theory showing that in a large class of spin - ½ quasiperiodic quantum kicked rotors, a dynamical analog of the integer quantum Hall effect (IQHE) emerges from an intrinsic chaotic structure. Specifically, the inverse of the Planck's quantum (h_e) and the rotor's energy growth rate mimic the `filling fraction' and the `longitudinal conductivity' in conventional IQHE, respectively, and a hidden quantum number is found to mimic the `quantized Hall conductivity'. We show that for an infinite discrete set of critical values of h_e, the long-time energy growth rate is universal and of order of unity (`metallic' phase), but otherwise vanishes (`insulating' phase). Moreover, the rotor insulating phases are topological, each of which is characterized by a hidden quantum number. This number exhibits universal behavior for small h_e, i.e., it jumps by unity whenever h_e decreases, passing through each critical value. This intriguing phenomenon is not triggered by the like of Landau band filling, well-known to be the mechanism for conventional IQHE, and far beyond the canonical Thouless-Kohmoto-Nightingale-Nijs paradigm for quantum Hall transitions. Instead, this dynamical phenomenon is of strong chaos origin; it does not occur when the dynamics is (partially) regular. More precisely, we find that, for the first time, a topological object, similar to the topological theta angle in quantum chromodynamics, emerges from strongly chaotic motion at microscopic scales, and its renormalization gives the hidden quantum number. Our analytic results are confirmed by numerical simulations. Our findings indicate that rich topological quantum phenomena can emerge from chaos

a. chaos b. turbulence c. frustration d. jiggling

Q33. Aharonov-Bohm phases in a quantum LC circuit: ChunJun Cao, Yuan Yao, and Ariel R. Zhitnitsky Walter Burke Institute for Theoretical Physics, California Institute of Technology, Pasadena, CA 91125, USA; Department of Physics and Astronomy, University of British Columbia, Vancouver, B.C. V6T 1Z1, Canada. We study novel types of contributions to the partition function of the Maxwell system deﬁned on a small compact manifold. These contributions, often not addressed in the perturbative treatment with physical photons, emerge as a result of tunnelling transitions between topologically distinct but physically identical vacuum winding states. These new terms give an extra contribution to the Casimir pressure, yet to be measured. We argue that this eﬀect is highly sensitive to a small external electric ﬁeld, which should be contrasted with the conventional Casimir eﬀect where the vacuum photons are essentially unaﬀected by any external ﬁeld. Furthermore, photons will be emitted from the vacuum in response to a time-dependent electric ﬁeld, similar to the dynamical Casimir eﬀect in which real particles are radiated from the vacuum due to the time-dependent boundary conditions. We also propose an experimental setup using a quantum LC circuit to detect this novel eﬀect. We expect physical electric charges to appear on the capacitor plates when the system dimension is such that coherent Aharonov-Bohm phases can be maintained over macroscopically large

a. steps b. distances c. spaces d. jumps

Q34. Published in Applied Physics Letters, Vol. 108, Iss.2 (2016) The phase transition in VO2 probed using x-ray, visible and infrared radiations: Suhas Kumar1, John Paul Strachan, A. L. David Kilcoyne, Tolek Tyliszczak, Matthew D. Pickett, Charles Santori, Gary Gibson and R. Stanley Williams: Email: John-Paul.Strachan@HP.com: Vanadium dioxide (VO2) is a model system that has been used to understand closely-occurring multiband electronic (Mott) and structural (Peierls) transitions for over half a century due to continued scientific and technological interests. Among the many techniques used to study VO2, the most frequently used involve electromagnetic radiation as a probe. Understanding of the distinct physical information provided by different probing radiations is incomplete, mostly owing to the complicated nature of the phase transitions. Here we use transmission of spatially averaged Infrared (λ=1.5 µm) and Visible (λ=500 nm) radiations followed by spectroscopy and nanoscale imaging using x-rays (λ=2.25-2.38 nm) to probe the same VO2 sample while controlling the ambient temperature across its phase transitions and monitoring its electrical resistance. We directly observed nanoscale puddles of distinct electronic and structural compositions during the transition. The two main results are that, during both heating and cooling, the transition of infrared and visible transmission occur at significantly lower temperatures than the Mott transition; and the electronic (Mott) transition occurs before the structural (Peierls) transition in temperature. We use our data to provide insights into possible microphysical origins of the different transition characteristics. We highlight that it is important to understand these effects because small changes in the nature of the probe can yield quantitatively, and even qualitatively, different results when applied to a non-trivial multiband phase transition. The phase transitions are

a. Sporadic. b. irregular. c. regular d. hysteretic

Q35.arXiv:1510.00286: Chimera-like states in modular neural networks: Dt. 1 Oct 2015 (v1), last revised 29 Nov 2015 (this version, v2)) JohanneHizanidis, Nikos E. Kouvaris, Gorka Zamora-López, Albert Díaz-Guilera, Chris G. Antonopoulos: Chimera-like states, namely the coexistence of coherent and incoherent behaviour, were previously analysed in complex networks. However, they have not been extensively studied in modular networks. Here, we consider a neural network inspired by the connectome of the C.elegans soil worm, organized into six interconnected communities, where neurons obey chaotic bursting dynamics. Neurons are assumed to be connected with electrical synapses within their communities and with chemical synapses across them. As our numerical simulations reveal, the coaction of these two types of coupling can shape the dynamics in such a way that chimera-like states can happen. They consist of a fraction of synchronized neurons which belong to the larger communities, and a fraction of desynchronized neurons which are part of smaller communities. In addition to the Kuramoto order parameter ρ, we also employ other measures of coherence, such as the chimera-like χ and meta-stability λ indices, which quantify the degree of synchronization among communities and in time, respectively. We perform the same analysis for networks that share common features with the C.elegans neural network. Similar results suggest that under certain assumptions, chimera-like states are prominent phenomena in modular networks, and might provide insight for the behaviour of more complex modular

a. Rings b. networks. c. netizens d. devices

Q36.arXiv:1601.06176: What is Information? Christoph Adami: email: adami@msu.edu: Abstract: Information is a precise concept that can be deﬁned mathematically, but its relationship to what we call “knowledge” is not always made clear. Furthermore, the concepts “entropy” and “information”, while deeply related, are distinct and must be used with care, something that is not always achieved in the literature. In this elementary introduction, the concepts of entropy and information are laid out one by one, explained intuitively, but deﬁned rigorously. I argue that a proper understanding of information in terms of prediction is key to a number of disciplines beyond engineering, such as physics and biology. A kind reviewer brought to my attention an elegant and insightful article by E.T. Jaynes, in which Jaynes not only accurately characterizes the diﬀerence between Boltzmann and Gibbs thermodynamic entropies and derives thermodynamics’ second law, but also makes essentially the same statement about entropy that I have made here, by writing: “From this we see that entropy is an anthropomorphic concept, not only in the well-known statistical sense that it measures the extent of human ignorance as to the microstate. Even at the purely phenomenological level, entropy is an anthropomorphic concept. For it is a property, not of the physical system, but of the particular experiments you or I choose to perform on it.” While this statement pertained to thermodynamics entropy, it applies just as well to Shannon entropy as the two are intimately related. Jaynes dissects this relationship cogently in his article and I see no need to repeat it here as my focus is on information, not entropy. I have written about the relationship between thermodynamic and Shannon entropy but wish I would have known then. Perhaps this link is best summarized by noting that thermodynamics is a special case of information theory where “all the fast things have happened, but the slow things have not” (as Richard Feynman described Thermodynamical equilibrium). In other words, in equilibrium information about the fast things has disappeared, but there may still be information about the things. [22 Jan 2016].

a. Average. b. fast c. slow d. rapid

Q37. hep-ph: 5 Jan 2016: Heavy Quark and Quarkonium Transport in High Energy Nuclear Collisions: Kai Zhou, Wei Dai, Nu Xu, Pengfei Zhuang, Abstract: The strong interaction between heavy quarks and the quark gluon plasma makes the open and hidden charm hadrons be sensitive probes of the deconﬁnement phase transition in high energy nuclear collisions. Both the cold and hot nuclear matter eﬀects change with the colliding energy and signiﬁcantly inﬂuence the heavy quark and charmonium yield and their transverse momentum distributions. The ratio of averaged quarkonium transverse momentum square and the elliptic ﬂow reveal the nature of the QCD medium created in heavy ion collisions at SPS, RHIC and LHC energies. Heavy quarks and quarkonia are sensitive probes of the quark gluon plasma created in high energy nuclear collisions, due to their strong interaction with the constituents of the hot medium. By taking into account the cold and hot nuclear matter eﬀects on their evolution in the partonic and hadronic phases, we can describe most of the experimental data by adjusting some parameters in phenological models. However, there exist still some puzzles which are beyond our expectations, like the simultaneous treatment of the heavy quark RAA and v2, the double ratio of ψ′ to J/ψ yield in some special rapidity, the strong charmonium enhancement in peripheral collisions, and the partial thermalization of charmonia in systems which are

a. Multiple. b. Small c. Great d. Big

Q38. (arXiv:1601.00642v1 [hep-ph]:Calculating Masses of Penta-quarks Composed of Baryons and Mesons: Narges Tazimi Majid Monemzadeh Shahnaz Babaghodrat: Department of Physics, University of Kashan, Kashan 87317-51167, I. R. Iran: Abstract: In this paper, we consider an exotic baryon (penta-quark) as a bound state of two-particle systems composed of a baryon (nucleon) and a meson. We used a baryon - meson picture to reduce a complicated ﬁve-body problem to two simpler two-body problems. The homogeneous Lippmann-Schwinger integral equation is solved in conﬁguration space by using Yukawa potential. We calculate the masses of penta-quarks θc(uudd ¯ c), θb(uudd ¯ b), θbs(buud ¯ s), and θcs(cuud ¯ s). We investigated penta-quark systems as hadronic composites of a meson and a nucleon. We used the Yukawa potential and solved Lippman Schwinger equation for systems consisting of mesons and baryons and obtained the masses of Penta-quarks in I = 0 state. Our results are in good agreement with previous research. According to our method, the solution of ﬁve-body systems is reduced to the solution of two-body systems without taking into account the relativistic corrections. We would like to claim that although this method is not a precise solution of the ﬁve-body system, its important advantage is the reduction of the complicated ﬁve-body problem to a ……………. problem. { Ῡ } Fill the gap!

a. Two-body b. three-body c. four-body d. one-body.

Q39. Relativistic Effects Break Periodicity in Group 6 Diatomic Molecules Yi-Lei Wang, Han- Shi Hu’, Wan- Lu Li, Fan Wei Jun Li’: Department of Chemistry & Key Laboratory of Organic Optoelectronics and Molecular Engineering of Ministry of Education, Tsinghua University, Beijing 100084, China. J. Am. Chem. Soc., January 19, 2016: huhanshi12@gmail.com, junli@mail.tsinghua.edu.cn, Abstract: The finding periodic law is a milestone in chemical science. The periodicity of light elements in the Periodic Table is fully accounted for by quantum mechanics. Here we report that relativistic–effects change the bond multiplicity of the group 6 diatomic molecules M, (M= Cr, Mo, W, Sg) from hexatuple bonds for Cr2, Mo2, W2, to quadruple bonds for Sg2, thus breaking the periodicity in the nonrelativistic domain. The same trend is also fund for other super-heavy element diatomics Rf2, Db2, Bh2, and Hs2. Bond order causes significant changes in the bond distance, vibrational frequencies, force constants and dissociation energies. Relativistic effects break the periodicity in the nonrelativistic domain derived for light element chemistry and novel properties are expected for chemical compounds of super-heavy

a. Mesons b. quarks c. elements d. devices

Q40. I believe there are “15, 747, 724, 136, 275 ,002, 577, 605, 653, 961, 181, 555, 468, 044, 717, 914, 527, 116, 709, 366, 231, 425, 076, 185, 631, 031, 296” protons in the universe and the same number of electrons." So wrote the English astrophysicist Sir Arthur Eddington in his book Mathematical Theory of Relativity (1923). Eddington arrived at this outrageous conclusion after a series of convoluted (and wrong!) calculations in which he first "proved" that the value of the so-called fine-structure constant was exactly 1/136. This value appears as a factor in his prescription for the number of particles (protons + electrons; neutrons were not discovered until 1930) in the universe: 2 × 136 × 2²⁵⁶ = 17 × 2²⁶⁰ = 3.149544... × 10⁷⁹ (double the number written out in full in the quote above). This is the Eddington number, notable for being the largest specific integer (as opposed to an estimate or approximation) ever thought to have a unique and tangible relationship to the physical world. Unfortunately, experimental data gave a slightly lower value for the fine-structure constant, closer to 1/137. Unfazed, Eddington simply amended his "proof" to show that the value had to be exactly 1/137, prompting the satirical magazine Punch to dub him "Sir Arthur Adding-One." New ways of writing seriously large numbers: hy(a, n, b) = { 1 + b for n = 0; { a + b for n = 1; { a × b for n = 2; { a↑b for n = 3
{ a↑↑b hy(a, 4, b-1) for n = 4; { hy(a, n-1, hy(a, n, b-1)) for n > 4; { a for n > 1, b = 1: Beyond hyper are other triadic operators capable of generating large numbers even faster. The Ackermann function and the Steinhaus-Moser notation are both equivalent to a triadic operator that is somewhat more powerful than hy(a, n, b). Similarly, Conway's chained-arrow notation marks an evolution of Knuth's symbolism. These various techniques and notations can produce immense finite numbers. But beyond any of these, lie the many different kinds of,

a. Infinity b. Finite numbers c. large entities d. small numbers.

Q41. Targeting new technologies: Firing calcium projectiles at a very heavy actinide target worked well for producing elements 114 to 118, but for even heavier elements the likelihood of creating a new element this way declines. An apparently simple solution would be to just fire more projectiles at the target. It took researchers more than two years to produce a tiny amount of berkelium used to make element 117, at Oak Ridge National Laboratory. Current accelerators hit the target with about 10¹²projectiles every second. But ‘hitting the target with an even higher number of projectiles would actually burn the target’, explains ORNL physicist Krzysztof Rykaczewski. And you can burn your detector, too. We need better technology to avoid this. You could also make the target much larger and spread the projectile beam over its larger area, he adds, but making these actinide targets is not easy. Synthesising the 20mg of berkelium used to produce element 117 took more than two years. The Superheavy Element Factory that is being built at Dubna might alleviate this problem, but ‘there will have to be another breakthrough in the next five years or so’, says Roberto. However, researchers remain positive. ‘Within one generation’s lifetime we will probably reach element 124,’ speculates Rykaczewski. Eric Scern, a chemistry historian at the University of California, Los Angeles, US, agrees: ‘Fifteen years ago it was inconceivable that anyone would ever get as far as we got.’ The hunt for new elements, he adds, has been and will be driving technology development. One idea to overcome the limitations of current heavy element synthesis techniques is to induce nuclear transfer reactions. If you fired uranium at a uranium target the nuclei will never fuse, explains GSI researcher Christoph DUllmann. But the colliding nuclei can exchange protons and neutrons when they collide. ‘In some cases that might lead to a product that happens to have, for example, 120 protons,’ Düllmann says. ‘This may be a path to access isotopes that are not reachable by fusion reactions. Calculations are fuzzy on exactly how much larger the periodic table can get. Physicist Richard Feynman predicted element 137 to be the limit. ‘The calculation is simply based on Einstein’s theory of relativity,’ says Scerri. When atomic nuclei get larger and larger the electrons have to go faster and faster as a result to avoid falling into the nuclei. Once you reach a certain size calculations predict that the electrons have to go faster than the speed a light – a physical impossibility. Other calculations predict this will happen much later, however, around element 170. While the four latest additions to the periodic table are highly radioactive and decay in less than a minute, scientists expect to find an island of stability centred at elements 120 or 126. These elements’ ‘magic’ proton numbers correspond to filled nuclear shells. Just as fully filled valence electron shells make elements such as the noble gases chemically inert, filled neutron or proton shells increase the nucleus’ stability. Researchers hope that Unbinilium’s or Unbihexium’s (element 126) doubly magic isotopes, containing both a magic proton number and a magic neutron number, would be even longer lived than their other isotopes, though half-life estimates vary wildly from a few minutes to millions of years. Researchers have already seen increasing stability of known super-heavy elements when in isotopes with neutron numbers closer to the magic 184. ‘The holy grail in super-heavy element synthesis is to reach this neutron number,’ says Düllmann. ‘But the problem is that we currently don’t have two nuclei that will give us a super-heavy element that also have that many …………..’

a. Protons b. Nucleii c. Neutrons d. Quarks.

Q42. arXiv:1602.04824: Mass and Metallicity Requirement in Stellar Models for Galactic Chemical Evolution Applications: Benoit Côté, Christopher West, Alexander Heger, Christian Ritter, Brian W. O'Shea, Falk Herwig, Claudia Travaglio, Sara Bisterzo. (15 Feb 2016). We used a one-zone chemical evolution model to address the question of how many metallicities and massive stars are required in grids of stellar models for galactic chemical evolution applications. We used a set of yields that includes seven masses between 13 and 30 Msun, 15 metallicities between 0 and 0.03 in mass fraction, and different remnant mass prescriptions. We ran several simulations where we sampled subsets of stellar models to explore the impact of different grid resolutions. Stellar yields from low- and intermediate-mass stars and from Type Ia supernovae have been included in our simulations, but with a fixed grid resolution. We compared our results with the stellar abundances observed in the Milky Way for O, Na, Mg, Si, S, K, Ca, Ti, and Mn. Our results suggest that the range of metallicity considered is more important than the number of metallicities within that range, which only affects our numerical predictions by about 0.1 dex (=10^x where x=0.1). We found that our predictions at [Fe/H] < -2 are very sensitive to the metallicity range and the mass sampling used for the lowest metallicity included in the set of yields. Variations between results can be as high as 0.8 dex, for any remnant mass prescription. At higher [Fe/H], we found that the required number of masses depends on the element of interest and on the remnant mass prescription. With a monotonic remnant mass prescription where every model explodes as a core-collapse supernova, the mass resolution induces variations of 0.2 dex on average. But with a remnant mass prescription that includes islands of non-explodability, the mass resolution can cause variations of about 0.2 to 0.7 dex depending on the choice of metallicity range. With such a prescription, explosive or non-explosive models can be missed if not enough masses are selected, resulting in over- or under-estimations of the mass ejected by massive stars.

a. Stars b. galaxies c. Suns d. Elements.

Q43. arXiv: 1602.04831: Evolution of dispersion in the cosmic deuterium abundance: Irina Dvorkin, Elisabeth Vangioni, Joseph Silk, Patrick Petitjean, Keith A. Olive:(Submitted on 15 Feb 2016). Deuterium is created during Bing Bang Nucleosynthesis, and, in contrast to the other light stable nuclei, can only be destroyed thereafter by fusion in stellar interiors. In this paper we study the cosmic evolution of the deuterium abundance in the interstellar medium and its dispersion using realistic galaxy evolution models. We find that models that reproduce the observed metal abundance are compatible with observations of the deuterium abundance in the local ISM and z ~ 3 absorption line systems. In particular, we reproduce the low astration factor which we attribute to a low global star formation efficiency. We calculate the dispersion in deuterium abundance arising from different structure formation histories in different parts of the Universe. Our model also predicts an extremely tight correlation between deuterium and metal abundances which could be used to measure the primordial deuterium abundance.

a. Depletion b. abundance c. exhaust d. percentage.

Q44. arXiv:1602.04865: The Most Luminous Supernovae, Tuguldur Sukhbold, Stan Woosley, (Submitted on 15 Feb 2016) Recent observations have revealed an amazing diversity of extremely luminous supernovae, seemingly increasing in radiant energy without bound. We consider here the physical limits of what existing models can provide for the peak luminosity and total radiated energy for non-relativistic, isotropic stellar explosions. The brightest possible supernova is a Type I explosion powered by a sub-millisecond magnetar. Such models can reach a peak luminosity of 2×1046 erg s−1 and radiate a total energy of 4×1052 erg. Other less luminous models are also explored, including prompt hyper-energetic explosions in red supergiants, pulsational-pair instability supernovae, and pair-instability supernovae. Approximate analytic expressions and limits are given for each case. Excluding magnetars, the peak luminosity is near 1×1044 erg s−1 for the brightest models. The corresponding limits on total radiated power are 3×1051 erg (Type I) and 1×1051 erg (Type II). A magnetar-based model for the recent transient event, ASASSN-15lh is presented that strains, but does not exceed the

a. Limits b. counts c. thresholds d. numerics

Q45. arXiv:1602.05050: Electromagnetic Afterglows Associated with Gamma-Ray Emission Coincident with Binary Black Hole Merger Event GW150914: Ryo Yamazaki, Katsuaki Asano, Yutaka Ohira:(Submitted on 16 Feb 2016):Fermi Gamma-ray Burst Monitor detected gamma-ray emission 0.4 sec after a binary black-hole merger event, GW150914. We show that the gamma-ray emission is caused by a relativistic outflow with Lorentz factor larger than 10. Subsequently debris outflow pushes ambient gas to form a shock, which is responsible for the afterglow synchrotron emission. We find that the fluxes of radio and optical afterglows increase from about 107 sec to at least ∼10 yr after the burst trigger. Further follow-up observations in the radio and optical/infrared bands are encouraged. Detection of afterglows will localize the sky position of the gravitational-wave and the gamma-ray emissions and it will support the ………………….. association between them.

a. Linear b. structural c. chemical d. physical

Q46. arXiv:1602.05140: Short Gamma-Ray Bursts from the Merger of Two Black Holes: Rosalba Perna, Davide Lazzati, Bruno Giacomazzo, (Submitted on 16 Feb 2016) Short Gamma-Ray Bursts (GRBs) are explosions of cosmic origin believed to be associated with the merger of two compact objects, either two neutron stars, or a neutron star and a black hole. The presence of at least one neutron star has long been thought to be an essential element of the model: its tidal disruption provides the needed baryonic material whose rapid accretion onto the post-merger black hole powers the burst. The recent tentative detection by the Fermi satellite of a short GRB in association with the gravitational wave signal GW150914 produced by the merger of two black holes has shaken this standard paradigm. Here we show that the evolution of two high-mass, low-metallicity stars with main sequence rotational speeds a few tens of percent of the critical speed eventually undergoing a weak supernova explosion can produce a short gamma-ray burst. The outer layers of the envelope of the last exploding star remain bound and circularize at large radii. With time, the disk cools and becomes neutral, suppressing the magneto-rotational instability, and hence the viscosity. The disk remains 'long-lived dead' until tidal torques and shocks during the pre-merger phase heat it up and re-ignite accretion, rapidly consuming the disk and powering the short burst of ,

a. Alpha-ray b. light ray c. gamma-ray d. beta-ray.

Q 47. arXiv:1602.05592 Mid-infrared interferometry of 23 AGN tori: On the significance of polar-elongated emission: N. Lopez-Gonzaga, L. Burtscher, K.R.W. Tristram, K. Meisenheimer, M. Schartmann: 17 Feb 2016.

Context. Detailed high resolution studies of AGN with mid-infrared (MIR) interferometry have revealed parsec-sized dust emission elongated in the polar direction in four sources.

Aims. Using a larger, coherently analysed sample of AGN observed with MIR interferometry, we aim to identify elongated mid-infrared emission in a statistical sample of sources. More specifically we wish to determine if there is indeed a preferred direction of the elongation and whether this direction is consistent with a torus-like structure or with a polar emission.
Methods. We investigate the significance of the detection of an elongated shape in the MIR emission by fitting elongated Gaussian models to the interferometric data at 12 um. We pay special attention to 1) the uncertainties caused by an inhomogeneous (u,v) coverage, 2) the typical errors in the measurements and 3) the spatial resolution achieved for each object.

Results. From our sample of 23 sources we are able to find elongated parsec-scale MIR emission in five sources: three type 2s, one type 1i and one type 1. Elongated emission in four of these sources has been published before; NGC5506 is a new detection. The observed axis ratios are typically around 2 and the position angle of the 12 um emission for all the elongated sources seems to be always closer to the polar axis of the system than to the equatorial axis. Two other objects, NGC4507 and MCG-5-23-16 with a reasonably well mapped (u,v) coverage and good signal-to-noise ratios, appear to have a less elongated 12 um emission.

Conclusions. Our finding that sources showing elongated mid-infrared emission are preferentially extended in polar direction sets strong constraints on torus models or implies that both the torus and the NLR/outflow region have to be modelled together. Especially also models used for SED fitting will have to be revised to include emissions.

a. Emission dust b. polar dust c. modelled dust d. arbitrary dust.

Q48. arXiv:1602.05630: Spectroscopic Binaries in the Orion Nebula Cluster and NGC 2264: Marina Kounkel, Lee Hartmann, John J. Tobin, Mario Mateo, John I. Bailey III., Meghin Spencer, (17 Feb 2016): We examine the spectroscopic binary population for two massive nearby regions of clustered star formation, the Orion Nebula Cluster and NGC 2264, supplementing the data presented by Tobin et al. (2009, 2015) with more recent observations and more extensive analysis. The inferred multiplicity fraction up to 10 AU based on these observations is 5.3±1.2% for NGC 2264 and 5.8±1.1% for the ONC; they are consistent with the distribution of binaries in the field in the relevant parameter range. Eight of the multiple systems in the sample have enough epochs to make an initial fit for the orbital parameters. Two of these sources are double-lined spectroscopic binaries, for them we determine the mass ratio. Our reanalysis of the distribution of stellar radial velocities towards these clusters presents a significantly better agreement between stellar and gas kinematics than was previously thought.

a. Thought b. endorsed c. presumed d. guessed.

Q49. arXiv:1602.05529: Modelling the Afterglow of GW150914-GBM: Brian J. Morsony, Jared C. Workman, Dominic M. Ryan: 17 Feb 2016): We model the afterglow of the Fermi GBM event associated with LIGO detection GW150914, under the assumption that the gamma-ray are produced by a short GRB-like relativistic outflow. We model GW150914-GBM as both a weak, on-axis short GRB and normal short GRB seen far off axis. Given the large uncertainty in the position of GW150914, we determine that the best chance of finding the afterglow is with the MWA, with the flux from an off-axis short GRB reaching 0.1 - 10 mJy at 150 MHz by 1 - 12 months after the initial event. At low frequencies, the source would evolve from a hard to soft spectrum over several months. The radio afterglow would be detectable for several months to years after it peaks, meaning the afterglow may still be detectable and increasing in brightness NOW. With a localization from the MWA, the afterglow would be detectable at higher radio frequencies with the ATCA and in X-rays Chandra or

a. AMM b. ZMM c. XMM d. YMM

Q50. arXiv:1602.03841:Tests of general relativity with GW150914. The LIGO Scientific Collaboration, the Virgo Collaboration 11 Feb 2016. The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final-remnant's mass and spin, determined from the inspiral and post-inspiral phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. The data following the peak of GW150914 are consistent with the least-damped quasi-normal-mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parameterized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and, bound, for the first time several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength in a hypothetical theory of gravity in which the graviton is massive and place a 90%-confidence lower bound of 1013 km. Within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity.

a. Galactic gravity. b. self-gravity c. gravitation. d. Gravity.

Q51. International Journal of Advancement in Remote Sensing, GIS and Geography:Vol 3, No 2 (2015) p.123-146: ANALYSING THE SPATIO-TEMPORAL LINK BETWEEN EARTHQUAKE OCCURRENCES AND ORBITAL PERTURBATIONS INDUCED BY PLANETARY CONFIGURATION: C. Jeganathan, G. Gnanasekaran, Tanushree Sengupta: The study has analysed the spatio-temporal positions (helio-centric and geo-centric) and configurations of all the planets on every day basis over the whole year 2015. Gravitational forces are invisible and undetectable, and hence it is very difficult to map the presence of these forces. The study has made a bold attempt in conceptualising indirect way of detecting spatial locations and understanding these gravity forces through earth quake events. The study has found that there are very clear evidences of planetary configuration creating hotspots of orbital perturbations which in-turn has some effect on Earth's orbital path which finally results in Earthquakes. The study analysed 10 different planetary configurations. The study claims that there are local gravitational interactions amongst bigger planets (Jupiter, Saturn, Uranus, Neptune) which creates an invisible resultant gravity vectors (IRGV) which acts as imperceptible planetary force when an inner planet crosses them. The study has estimated the locations of those invisible forces and analysed their links with major earthquakes (>6.0 only). This study has revealed that whenever Earth crossed these IRGVs invariably there were major EQs, and other inner planetary crossings as well showed similar results. Mercury and Moon being the fastest moving objects in the sky they act as catalyst when there is other planetary perturbing configuration. Overall the explanation capabilities of each of possible configurations were critically cross checked and hope that the study will give a New Dimension in the field of Earthquake, Gravity anomalies and their prediction. Finally, the study predicted the sensitive days for the year 2016 and researchers may validate our concepts and results based on actual ground,

a. Perturbation b. turbulence. c. Shaking. d. Vibration

Q52. DETAILS OF THE SPATIAL STRUCTURE AND KINEMATICS OF THE CASTOR AND URSA MAJOR STREAMS: S.V. Vereshchagin1, N.V. Chupina1 1 Institute of Astronomy of the Russian Academy of Sciences (INASAN), 48 Pyatnitskaya st., Moscow, Russia; svvs@ya.ru: Received: 2015 July 2; accepted: 2015 December 15: Abstract. A list of the Castor stream members is compiled based on the data from various authors. The membership probabilities for some stars are revised based on the individual apex, multiplicity, observational errors, and peculiarity. The apex of the Castor moving group is determined using the apex diagram method. The parameters of the Castor and Ursa Major streams are compared and the positions of the two streams on the apex diagram are found to diﬀer by 225◦, implying that the two groups move in almost opposite directions. Stars of both moving groups are intermixed in space, the Castor stream occupies a smaller volume than UMa stream and is located inside it. Our results can be useful for understanding the morphology of the Galactic disk in the Sun’s vicinity. We investigate the Castor and Ursa Major (UMa) streams, which are the closest to the Sun and therefore may provide insight into the structure of the Galactic disk in the solar vicinity. A feature of both streams is that they have many multiple systems, some of which consist of up to six stars! For example, the UMa stream contains a sextuple system, which includes Mizar and Alcor (Mamajek et al. 2010) and, perhaps HD 76644 (Zhuchkov et al. 2006). Moreover, UMa stream contains three kinematic groups. Castor group, after four iterations we ﬁnd A = 79.33◦, D = −15.06◦ based on the data for about stars

a. 65 b. 100 c.15 d. 20

Q53. New Bi-Gravity from New Massive Garvity A. Akhavana, M. Alishahihab, A. Naseha, A. Nematic and A. Shirzadc, Thu, 10 Mar 2016 13:56:26 GMT (146kb,D): High Energy Physics - Theory (hep-th); General Relativity and Quantum Cosmology (gr-qc) arXiv:1603.03270 [hep-th] Using the action of three dimensional New Massive Gravity (NMG) we construct a new bi-gravity in three dimensions. This can be done by promoting the rank two auxiliary ﬁeld appearing in the expression of NMG’s action into a dynamical ﬁeld. We show that small ﬂuctuations around the AdS vacuum of the model are nontachyonic and ghost free within certain range of the parameters of the model. We study central charges of the dual ﬁeld theory and observe that in this range they are positive too. This suggests that the proposed model might be a consistent three dimensional bi-gravity. We note, however, that for a particular value of parameters the spin-2 ﬁeld becomes partially massive which means that in the linearized level it has just one degree of freedom. Of course we would expect that this reduction of degrees of freedom is an artifact of the linear approximation. Accepting this fact we would like to conclude that the NBG model has the same degrees of freedom as that of NMG and therefore could be thought of as a model which addresses solution of bulk-boundary clash for NMG. Intuitively it is simple to see how our model could resolve bulk-boundary clash. Indeed we have shown that upon linearization the quadratic part of the action contains two parts: one for a massless graviton and one for a massive spin-2 ﬁeld. Denoting the coeﬃcients of these terms by A0 and Am, respectively, one can see that for NMG model these two factors cannot be positive. Moreover since A0 is related to the central charge of the dual theory one generally gets the bulk-boundary clash. Whereas for the NBG model there is a range of parameters where both A0 and Am can be positive

a. instantly b. arbitrarily c. simultaneously d. randomly

Q54. DISCRETE QUANTUM GRAVITY and QUANTUM FIELD THEORY: S. Gudder Department of Mathematics University of Denver Denver, Colorado 80208, U.S.A. sgudder@du.edu; Tue, 8 Mar 2016 02:01:02 GMT (20kb): Mathematical Physics (math-ph); High Energy Physics - Theory (hep-th) arXiv:1603.03471: Abstract: We introduce a discrete 4-dimensional module over the integers that appears to have maximal symmetry. By adjoining the usual Minkowski distance, we obtain a discrete 4-dimensional Minkowski space. Forming universe histories in this space and employing the standard causal order, the histories become causal sets. These causal sets increase in size rapidly and describe an inﬂationary period for the early universe. We next consider the symmetry group G for the module. We show that G has order 24 and we construct its group table. In a sense G is a discrete approximation to the Lorentz group. However, we note that it contains no boosts and is essentially a rotation group. Unitary representations of G are constructed. The energy-momentum space dual to the discrete module is obtained and a quantum formalism is derived. A discrete Fock space is introduced on this structure and free quantum ﬁelds are considered. Finally, we take the ﬁrst step in a study of interacting quantum

a. Fields b. vortices c. fluids d. vertices.

Q55. Dt. 11 Mar 2016: The ultimate absorption at light scattering by a single obstacle. Andrey E. Miroshnichenko Australia Michael I. Tribelsky, Russia (Dated: March 14, 2016): Based on fundamental properties of light scattering by a particle we reveal the existence of the ultimate upper limit for the light absorption by any partial mode. First, we obtain this result for scattering of a plane wave by a symmetric spherical or inﬁnite cylindrical structure of an arbitrary radius. Then, we generalize it to an arbitrary ﬁnite obstacle. Importantly, the result is true for any polarization, any angle of incidence of the plane wave and any type of the structure (homogeneous, stratiﬁed, or with smoothly variable refractive index). The corresponding maximal partial crosssection is a universal quantity, which does not depend on the optical constants of the scatterer its radius, and even its shape. The corresponding maximal partial scattering cross-section is given by the following simple expression: σ ^(l) _{abs
max} = (2l + 1)π/ 2k² where l stands for the multipolarity of the plasmonic resonance (l = 1 — dipolar, l = 2 — quadrupolar, etc.) and k designates the wavenumber of the incident light in a [ σ ^(l) _{abs max} = (2l + 1)π/ 2k²]

a. Vacuum b. Space c. water d. gas.

Q56. arXiv:1603.04858: astro-ph.CO: Iron in galaxy groups and clusters: Confronting galaxy evolution models with a newly homogenized dataset. Authors: Roberts M. Yates, Peter A. Thomas, Bruno M. B. Henrigues, (15 Mar 2016). Abstract: We present an analysis of the iron abundance in the hot gas surrounding galaxy groups and clusters. To do this, we first compile and homogenize a large dataset of 79 low-redshift (|z| = 0.03) systems (159 individual measurements) from the literature. Our analysis accounts for differences in aperture size, solar abundance, and cosmology, and scales all measurements using customized radial profiles for the temperature (T), gas density, and iron abundance (Z). We then compare this dataset to groups and clusters in the L-Galaxies galaxy evolution model. Our homogenized dataset reveals a tight T-Z relation for clusters, with a scatter in Z of only 0.10 dex and a slight negative gradient. After examining potential measurement biases, we conclude that at least some of this negative gradient has a physical origin. Our model suggests greater accretion of hydrogen in the hottest systems, via stripping of gas from in falling satellites, as a cause. At lower temperatures, L-Galaxies over-estimates Z in groups, indicating that metal-rich gas removal (via e.g. AGN feedback) is required. L-Galaxies provides a reasonable match to the observed Z in the intracluster medium (ICM) of the hottest clusters from at least z ~ 1.3 to 0.3. This is achieved without needing to modify any of the galactic chemical evolution (GCE) model parameters. However, the Z in intermediate-temperature clusters appears to be under-estimated in our model at z = 0. The merits and problems with modifying the GCE modelling to correct this are

a. Discussed b. observed c. modelled d. suggested.

Q57. March 17, 2016: Are Infrared Dark Clouds Really Quiescent? Authors: S. Feng, H. Beuther, Q. Zhang, Th. Henning, H. Linz, S. Ragan, R. Smith:Context. The dense, cold regions where high-mass stars form are poorly characterised, yet they represent an ideal opportunity to learn more about the initial conditions of high-mass star formation (HMSF), since high-mass starless cores (HMSCs) lack the violent feedback seen at later evolutionary stages. Aims. To investigate the initial conditions of HMSF by studying the dynamics and chemistry of HMSCs. Methods. We present continuum maps obtained from the Sub-millimeter Array (SMA) interferometry at 1.1mm for four infrared dark clouds (IRDCs, G28.34S, IRDC18530, IRDC18306, and IRDC18308). For these clouds, we also present line surveys at 1mm/3mm obtained from IRAM 30m single-dish observations. Results. (1) At an angular resolution of 2’’ (∼10+E04 AU at an average distance of 4 kpc), the 1.1mm SMA observations resolve each source into several fragments. The mass of each fragment is on average > 10M
, which exceeds the predicted thermal Jeans mass of the whole clump by a factor of up to 60, indicating that thermal pressure does not dominate the fragmentation process. Our measured velocity dispersions in the 30m lines imply that non-thermal motions provides the extra support against gravity in the fragments. (2) Both non-detection of high-J transitions and the hyperﬁne multiplet ﬁt of N2H+ (J = 1→0), C2H (N = 1→0), HCN (J = 1→0), and H(+13E+01)CN (J = 1→0), indicate that our sources are cold and young. However, obvious detection of SiO and the asymmetric line proﬁle of HCO+ (J=1→0) in G28.34S indicate a potential proto-stellar object and probable in fall motion. (3). With a large number of N-bearing species, the existence of carbon rings and molecular ions, and the anti-correlated spatial distributions between N2H+/NH2D and CO, our large-scale high-mass clumps exhibit similar chemical features as small-scale low-mass pre-stellar objects. Conclusions. This study of a small sample of IRDCs illustrates that thermal Jeans instability alone cannot explain the fragmentation of the clump into cold (T∼15 K), dense (> 105 cm−3) cores and that these IRDCs are not completely quiescent.

a. Reliable b. corrigible c. quiescent d. stable

Q58. arXiv.1603.05076: 29 Feb 2016: New analysis for the correlation between gravitational waves and neutrino detectors during SN1987A Authors: P. Galeotti, G. Pizzella: Abstract: The two major problems, still associated with the SN1987A, are: a) the signals observed with the gravitational waves detectors, b) the duration of the collapse. Indeed, the sensitivity of the gravitational wave detectors seems to be small for detecting gravitational waves and, while some experimental data indicate a duration of order of hours, most theories assume that the collapse develops in a few seconds. Since recent data of the X-ray NuSTAR satellite show a clear evidence of an asymmetric collapse, we have revisited the experimental data recorded by the underground and gravitational wave detectors running during the SN1987A. New evidence is shown that conﬁrms previous results, namely that the data recorded by the gravitational wave detectors running in Rome and in Maryland are strongly correlated with the data of both the Mont Blanc and the Kamiokande detectors, and that the correlation extends over a long period of time (one or two hours) centred at the Mont Blanc time. This result is obtained by comparing six independent ﬁles of data recorded by four diﬀerent experiments located at intercontinental distances. The signals of the GW detectors preceded the signals of the underground detectors by a time of the order of one second. We conclude that this new analysis of the experimental data obtained with the gravitational waves and neutrino detectors, strongly enforces the idea that between 2 and 4 hours UT of 23rd February 1987 both the neutrino and the GW bar-detectors were invested by intense ﬂuxes of particles and ﬁelds presumably originating from the SN1987A. As well known, higher ﬂuxes of particles continued until 7.35 UT not detected by the gravitational waves detectors and with only two interactions detected by the LSD experiment al 7h 36 m UT. Obviously, something has changed in the structure and dynamics of the collapsing core in this 4.7 hours-time interval between the ﬁrst neutrino burst and the second

a. Quark burst b. neutrino burst c. flux d. emissions.

Q59. [gr-qc] 16 March 2016: LIGO GW 150914 Gravitational Wave Detection and Generalized Gravitation Theory (MOG): J. W. Moﬀat: Ontario N2L 2Y5, Canada and Ontario N2L 3G1, Canada: March 17, 2016: Abstract: The nature of gravitational waves in a generalized gravitation theory is investigated. The linearized ﬁeld equations and the metric tensor quadrupole moment power and the decrease in radius of an in-spiralling binary system of two compact objects are derived. The generalized Kerr metric describing a spinning black hole is determined by its mass M and the spin parameter a=cS/G_NM². Using a generalized gravitational theory (MOG), the gravitational wave source GW 150914 data is ﬁtted by a binary black hole system with the masses m1 ∼ 10M⊙ and m2 ∼ 8M⊙, compared with the masses estimated by the LIGO-Virgo collaboration using general relativity, m1 ∼ 36M⊙ and m2 ∼ 29M⊙. It is argued that the smaller binary black hole masses accommodated by the generalized theory are in agreement with the current electromagnetic, observed X-ray binary upper bound for a black hole mass, M ∼ 10M⊙, so the ﬁnal quiescent black hole mass after the ring-down phase will be M ∼ 17M⊙, compared with the general relativity prediction M ∼ 62M⊙, after energy loss from gravitational radiation. The ﬁnal spin parameters for the binary components are expected to be a≤ 0.7. The reduced masses of the in-spiralling black holes are consistent with the observed black hole masses identiﬁed through electromagnetic observations. The GW 150914 source lies at a luminosity distance of 410⁺¹⁶⁰₋₁₈₀ Mpc corresponding to a redshift z = 0.09^+0.03_−0.04. The inferred initial black hole masses are m1 = 36⁺⁵₋₄ M⊙ and m2 = 29⁺⁴₋₄ M⊙, the ﬁnal black hole mass is M = 62⁺⁴₋₄M⊙, with 3.0^+0.5_−0.5M⊙c² energy radiated away in gravitational waves, and the ﬁnal black hole spin inferred from GR is a=0.67^+0.05_−0.07. The gravitational wave luminosity determined from GR reached a peak value of 3.6^+0.5 _−0.4 ×10⁵⁶ erg/s equivalent to 200⁺³⁰₋₂₀M⊙c²/s. The GW 150914 gravitational wave detection points to it being produced by the coalescence of two black holes - their orbital in-spiral and merger and ﬁnal black hole ring-down. During the period of 0.2 s, the detected signal increases in frequency and amplitude from about 8 cycles from 35 Hz to a maximum 150 Hz. The merging of the black holes requires a numerical solution of the GR ﬁeld equations. This has been accomplished for GR and solutions have been derived that can match the GW 150914 wave form signal. Future work will require that numerical solutions to the generalized gravitational ﬁeld equations be obtained, leading to the determination of gravitational wave

a. Shapes b. kinks c. forms d. jumps.

Q60. High Energy Physics, Phenomenology (hep-hp) arXiv:1603.0467. Active galaxies may harbour wormholes if dark matter is axionic: Konstantinos Dimopoulos, Lancaster LA1 4YB, UK, March 16, 2016, Abstract: AGN jets carry helical magnetic ﬁelds, which can aﬀect dark matter if the latter is axionic. This preliminary study shows that the nature of the axionic condensate may change and instead of dark matter may behave more like exotic matter, which violates the null energy condition. If the central supermassive black hole of an active galaxy is laced with exotic matter then it may become a wormhole. In general, the presence of exotic matter may aﬀect galaxy formation and galactic dynamics, so this possibility should not be ignored when considering axionic dark matter. As a corollary, if dark matter is axionic, one can imagine that an advanced civilisation may generate artiﬁcially a helical magnetic ﬁeld, with the appropriate characteristics to alter the nature of the local dark matter into exotic matter. This might become a way to realise interstellar travel (and/or time travel} since It may to give rise to a wormhole.

a. Exotic matter b. null conditions c. helical steps d. wormhole

Q61. A Survey on High-Speed Railway Communications: A Radio Resource Management Perspective. Authors: Shengfeng Xu, Gang Zhu, Bo Ai, Zhangdui Zhong. Information Theory (cs.IT) High-speed railway (HSR) communications will become a key feature supported by intelligent transportation communication systems. The increasing demand for HSR communications leads to signiﬁcant attention on the study of radio resource management (RRM), which enables efﬁcient resource utilization and improved system performance. RRM design is a challenging problem due to heterogenous quality of service (QoS) requirements and dynamic characteristics of HSR wireless communications. The objective of this paper is to provide an overview on the key issues that arise in the RRM design for HSR wireless communications. A detailed description of HSR communication systems is ﬁrst presented, followed by an introduction on HSR channel models and characteristics, which are vital to the cross-layer RRM design. Then we provide a literature survey on state-of-the-art RRM schemes for HSR wireless communications, with an in-depth discussion on various RRM aspects including admission control, mobility management, power-control and resource allocation. Finally, this paper outlines the current challenges and open issues in the area of RRM design for HSR wireless communications. Radio resource management is a powerful tool that enables high resource utilization and results in improved QoS performance. However, compared with common cellular communications, some characteristics in HSR wireless communications, such as high mobility, unique channel conditions and heterogenous QoS requirements, impose some challenges to the RRM design. This leads to signiﬁcant attention on the study of RRM under HSR scenarios. In this paper, we have provided a literature survey on HSR wireless communications from a perspective of RRM design. Firstly, we have presented an overview of the HSR communication systems with a detailed description of network architecture, railway applications and services as well as advanced transmission technologies. Then the HSR channel models and characteristics are introduced, which are vital to the cross-layer RRM design and optimization. Afterwards, we have surveyed the RRM schemes for HSR wireless communications, with an in-depth discussion on admission control, mobility management, power-control and resource

a. Restrictions b. Optimization c. Decentralization d. Allocation.

Q62. THE VERY MASSIVE STAR CONTENT OF THE NUCLEAR STAR CLUSTERS IN NGC 5253 by L. J. Smith, P. A. Crowther, D. Calzetti, and F. Sidoli: Draft version March 24, 2016: ABSTRACT: The blue compact dwarf galaxy NGC 5253 hosts a very young starburst containing twin nuclear star clusters, separated by a projected distance of 5 pc. One cluster (#5) coincides with the peak of the Hα emission and the other (#11) with a massive ultra-compact HII region. A recent analysis of these clusters shows that they have a photometric age of 1 ± 1 Myr, in apparent contradiction with the age of 3–5 Myr inferred from the presence of Wolf-Rayet features in the cluster #5 spectrum. We examine Hubble Space Telescope ultraviolet and Very Large Telescope optical spectroscopy of #5 and show that the stellar features arise from very massive stars (VMS), with masses greater than 100 M, at an age of 1–2 Myr. We further show that the very high ionizing ﬂux from the nuclear clusters can only be explained if VMS are present. We investigate the origin of the observed nitrogen enrichment in the circum-cluster ionized gas and ﬁnd that the excess N can be produced by massive rotating stars within the ﬁrst 1 Myr. We ﬁnd similarities between the NGC 5253 cluster spectrum and those of metal poor, high redshift galaxies. We discuss the presence of VMS in young, star-forming galaxies at high redshift; these should be detected in rest frame UV spectra to be obtained with the James Webb Space Telescope. We emphasize that population synthesis models with upper mass cut-oﬀs greater than 100 M⊙ are crucial for future studies of young massive star clusters at all redshifts. We compare the UV spectrum of cluster #5 with those of metal poor, high redshift galaxies and show that it has many similarities in terms of the HeII emission line strength and width, and the presence of strong OIII] λλ1661,1666 and CIII] λλ1907,1909 nebular emission. VMS may exist in young star-forming regions at high redshift and their presence should be revealed by UV rest frame spectra to be obtained by JWST. Population synthesis models typically have upper mass cut-oﬀs of 100 M⊙. It is crucial to extend these into the VMS regime to correctly account for the radiative, mechanical and chemical feedback, which will be dominated by VMS for the ﬁrst 1–3 Myr in star-forming regions.

a. Clusters b. regions c. areas d. red-shifts.

Q63. Solar & Stellar Astrophysics: OBSERVATION OF THE EVOLUTION OF A CURRENT SHEET IN SOLAR FLARE: Chunming Zhu, Rui Liu, David Alexander, R.T. James McAteer: ABSTRACT: We report multi-wavelength and multi-viewpoint observations of a solar eruptive event which involves loop-loop interactions. During a C2.0 ﬂare, motions associated with inﬂowing and outﬂowing plasma provide evidence for ongoing magnetic reconnection. The ﬂare loop top and a rising “concaveup” feature are connected by a current-sheet-like structure (CSLS). The physical properties (thickness, length, temperature, and density) of the CSLS are evaluated. In regions adjacent to the CSLS, the EUV emission (characteristic temperature at 1.6 MK) begins to increase more than ten minutes prior to the onset of the ﬂare, and steeply decreases during the decay phase. The reduction of the emission resembles that expected from coronal dimming. The dynamics of this event imply a magnetic reconnection rate in the range 0.01 – 0.05. Our study reveals several important physical properties of the CSLS in loop-loop interaction. First, the length of the CSLS appeared to grow slowly with an average speed of ∼11 km s−1. The extension of the current sheet is expected during solar ﬂares, and can grow as fast as a few hundred km s−1 in the wake of an erupting CME (Forbes & Lin 2000; Savage et al. 2010). The low growth speed here might be related to a diﬀerent scenario, i.e. loop-loop interaction. Second, the observed erupting SHL, which initiated along with the downward shrinking loops, and appeared intermittently with an average velocity of ∼150 km s−1, might be related to the outward ﬂows/blobs in current sheet (e.g., Shen et al. 2011). Third, the emission in AIA 193 ˚A adjacent to the CSLS ﬁrst increased, before its steep reduction in the late stage of the ﬂare. This reduction in the emission is suggestive of the coronal dimmings frequently reported in association with CMEs (e.g., Sterling & Hudson 1997; Zarro et al. 1999). In the present case, the dimmings are reported to result from a loop-loop interaction without evident detection of a CME. The relationship between the earlier increase in emission and the onset of the ﬂare, if any, needs to be investigated in future

a. Research b. investigations c. explorations d. studies.

Q64. Materials Science: Black Phosphorus Mid-Infrared Photodetectors with High Gain: Qiushi Guo, Andreas Pospischil, Maruf Bhuiyan, Hao Jiang, He Tian, Damon Farmer, Bingchen Deng, Cheng Li, Shu-Jen Han, Han Wang, Qiangfei Xia, Tso-Ping Ma, Thomas Mueller, and Fengnian Xia: ABSTRACT: Recently, black phosphorus (BP) has joined the two-dimensional material family as a promising candidate for photonic applications, due to its moderate bandgap, high carrier mobility, and compatibility with a diverse range of substrates. Photodetectors are probably the most explored BP photonic devices, however, their unique potential compared with other layered materials in the mid-infrared wavelength range has not been revealed. Here, we demonstrate BP mid-infrared detectors at 3.39 µm with high internal gain, resulting in an external responsivity of 82 A/W. Noise measurements show that such BP photodetectors are capable of sensing low intensity mid-infrared light in the pico-watt range. Moreover, the high photo-response remains effective at kilohertz modulation frequencies, because of the fast carrier dynamics arising from BP’s moderate bandgap. The high photo-response at mid-infrared wavelengths and the large dynamic bandwidth, together with its unique polarization dependent response induced by low crystalline symmetry, can be coalesced to promise photonic applications such as chip-scale mid-infrared sensing and imaging at low light levels. In conclusion, a sensitive MWIR photodetector based on a black phosphorus transistor has been demonstrated at 3.39 μm, capable of performing low power detection in pico-watts range. The device exhibits high photoconductive gain and dynamic bandwidth in kHz range. Moreover, BP’s capability to resolve incident light polarization adds another degree of freedom to photo-detection

a. Instruments b. Devices c. gadgets d. units

Q65. Direct Observation of the Skyrmion Hall Effect: Wanjun Jiang, Xichao Zhang2, Guoqiang Yu, Wei Zhang, M. Benjamin Jungfleisch, John E. Pearson, Olle Heinonen, Kang L. Wang, Yan Zhou, Axel Hoffmann, Suzanne G. E. te Velthuis: ABSTRACT: The well-known Hall effect describes the transverse deflection of charged particles (electrons/holes) in an electric-current carrying conductor under the influence of perpendicular magnetic fields, as a result of the Lorentz force. Similarly, it is intriguing to examine if quasi-particles without an electric charge, but with a topological charge, show related transverse motion. Chiral magnetic skyrmions with a well-defined spin topology resulting in a unit topological charge serve as good candidates to test this hypothesis. In spite of the recent progress made on investigating magnetic skyrmions, direct observation of the skyrmion Hall effect in real space has, remained elusive. Here a current-induced spin Hall spin torque, we experimentally observe the skyrmion Hall effect by driving skyrmions from creep motion into the steady flow motion regime. We observe a Hall angle for the magnetic skyrmion motion as large as 𝟏𝟓⁰ for current densities smaller than 𝟏𝟎𝟕 𝐀/𝐜𝐦^𝟐 at room temperature. The experimental observation of transverse transport of skyrmions due to topological charge may potentially create many exciting opportunities for the emerging field of skyrmionics, including novel applications such as topological selection. In the future, similar to the well-studied motion of superconducting vortex in the presence of pinning35, by tailoring the geometry/distribution of materials defects or artificially created pinning sites, it will be possible to experimentally reveal many exciting phenomena such as dynamic phase transitions, rectifying motion of skyrmions from ratchets, and quantized transport of magnetic skyrmions. Our observations also indicate that the topological charges of magnetic skyrmions, in combination with the current induced spin Hall spin torque, can be potentially integrated for realizing novel functionalities, such as topological,

a. Sorting b. analysis c. ordering d. grouping.

Q66. Mesoscale and Nanoscale Physics: Quantum time mirrors: Phillipp Reck, Cosimo Gorini, Arseni Goussev, Viktor Krueckl, Mathias Fink, Klaus Richter: ABSTRACT: Both metaphysical and practical considerations related to time inversion have intrigued scientists for generations. Physicists have strived to devise and implement time-inversion protocols, in particular diﬀerent forms of “time mirrors” for classical waves. Here we propose two conceptually diﬀerent realisations of instantaneous time mirrors for quantum systems, i.e. controlled time discontinuities acting through pulses on wave fronts and leading to distinct wave function echoes with high ﬁdelities. The ﬁrst concept exploits up to now unrelated mechanisms of wave front time inversion and population reversal in spatially extended two-level systems, the latter quintessential to spin echoes. It can be implemented in Dirac-like systems, such as (real or artiﬁcial) graphene. The second protocol is based on a non-linear mirror for a Bose-Einstein condensate whose dynamics is described by the non-linear Schro¨dinger equation, and is realisable in cold atom setups. The analytical and numerical considerations presented in this work conﬁrm the principles behind both QTMs. In the case of QTM for pseudo-relativistic graphene-like systems, this means that a suﬃciently fast and spatially homogeneous perturbation which opens a gap in a Dirac system can act similar to a microwave π pulse in spin-echo experiments, eﬀectively t-inverting the orbital wave function dynamics and thus generating a wave function echo. Topological insulators open up the intriguing perspective to unify the two mechanisms of spin-echo and orbital echo: States at the surface of a 3D topological insulator are governed by an eﬀective Dirac equation similar to graphene where, most notably, the electron spin takes the role of graphene pseudospin. This implies that the QTM concept presented here provides a simultaneous echo in the combined Hilbert space of spin and spatial degree of freedom. In the Bose-Einstein condensate QTM, the crucial aspect is instead the dominance of the interaction-induced nonlinearity over free propagation for a brief time interval. Both QTM mechanisms are thus based on distinctly diﬀerent concepts, yet they both achieve instantaneous t-inversion of a wave function with high ﬁdelity. As such, they are quantum counterparts of the instantaneous time mirror for water waves very recently realised by V. Bacot et al., however relying on a diﬀerent set of principles. Various experimental realisations of the QTMs proposed here can be imagined. For Dirac systems our QTM represents a general proof of concept, based on a single-particle picture and including the assumption that the inelastic relaxation time of the injected wave packet is larger than t₀. This condition might still be restrictive in real graphene, suggesting that some form of artiﬁcial graphene could be rather amenable to a straightforward experimental implementation of the QTM. On the other hand we demonstrated that the t-inversion protocol is fairly robust to elastic disorder and practically insensitive to pulse (gap) disorder. More generally, in analogy to the spin echo, QTM-based echo spectroscopy could be used as a probe of elastic and inelastic scattering times in Dirac-type 2D crystals. For the non-linear QTM we provide an estimate for values of the dimensionless relevant parameters σ and k, accessible in laboratory experiments with ultra-cold lithium atoms. The mass of a ⁷Li atom is m = 7.016u = 1.165 × 10⁻²⁶ kg. Taking the wave packet propagation time until the non-linear kick to be t₀ = 10ms, we see that the wave packet width range of 10 – 50 µm corresponds to 1.05 < σ < 5.26, and the mean velocity range of 2−10 mms⁻¹ corresponds to 2.1 < k < 10.5. These parameter ranges coincide with the ones considered in this article, which strongly suggests that the matter wave reversal eﬀects predicted here can be realised e.g. in experiments with lithium Bose-Einstein

a. observations b. findings c. condensates d. exclusions

Q67. If α, β are the eccentric angles of the ends of a focal chord of the ellipse

x^2/a^2 + y^2/b^2 = 1, then the eccentricity of the ellipse is

(sin α - sinβ ) / sin (α + β ) b. (sin α + sin β) / sin( α + β )

c. (cos α + cos β) / cos(α+ β ) d. (cos α + cos β )/ cos(α-β)

Q68. An ellipse has eccentricity ½ and one focus at S( ½ , 1). If one directrix is the common tangent, near to S, to the circle x^2+y^2=1 and x^2 – y2 =1. Then the equation of the ellipse is

a. 9(x-1/3)^2 + 12(y-1)^2=1 b. 12(x-1/3)^2 + 9(y-1)^2 =1

c. (1/12) * (x-1/2)^2 + 1/9 * (y-1)^2 =1 d. 3(x+1/2)^2 + 4(y-1)^2 =1.

Q69. The product of perpendiculars from the foci on any tangent to the ellipse

x^2/a^2 + y^2/b^2 = 1 is

a. a b. a^2 - b^2 c. b^2 d. sqrt(a^2 + b^2)

Q70. If lx + my+ n=0 is equation of line joining the extremities of pair of semi conjugate diameters of ellipse x^/a^2 + y^2/b^2 = 1 then (9 l^2 + 4 m^2)/n^2 equals

a. 1 b. 2.0 c. 1 d. 2.

Q71. Particle Acceleration in Solar Flares and Associated CME Shocks: Vah´e Petrosian, Stanford, CA 94305, USA. ABSTRACT: Observations relating the characteristics of electrons seen near Earth (SEPs) and those producing ﬂare radiation show that in certain (prompt) events the origin of both population appears to be the ﬂare site, which show strong correlation between the number and spectral index of SEP and hard X-ray radiating electrons, but in others (delayed), which are associated with fast CMEs, this relation is complex and SEPs tend to be harder. Prompt event spectral relation disagrees with that expected in thick or thin target models. We show that using a more accurate treatment of the transport of the accelerated electrons to the foot-points and to the Earth can account for this discrepancy. Our results are consistent with those found by Chen & Petrosian (2013) for two ﬂares using non-parametric inversion methods, according to which we have weak diﬀusion conditions, and trapping mediated by magnetic ﬁeld convergence. The weaker correlations and harder spectra of delayed events can come about by re-acceleration of electrons in the CME shock environment. We describe under what conditions such a hardening can be achieved. Using this (acceleration at the ﬂare and re-acceleration in the CME) scenario we show that we can describe the similar dichotomy that exists between the so called impulsive, highly enriched (³He and heavy ions) and softer SEP events, and stronger more gradual SEP events with near normal ionic abundances and harder spectra. These methods can be used to distinguish the acceleration mechanisms and to constrain their characteristics. Electrons produce hard X-rays (HXR) via non-thermal bremsstrahlung (NTB) and microwaves via synchrotron mechanisms in the lower solar atmosphere and type III (and other radio) bursts in the upper corona and beyond. Accelerated protons (and other ions) interacting with background ions result in de-excitation nuclear lines in the 1 to 7 MeV range, neutrons, and Pions which decay into (mainly) > 70 MeV gamma-rays. However, most of the energy of <∼ 100 MeV electrons and <∼ 1 GeV protons goes into heating and evaporation of the ﬂare plasma which then gives rise to thermal radiation from soft X-rays (SXR) to range of order,

a. Centimetre b. sub-millimetre c. Angstrom d. metre

Q72. Constraints on interacting dark energy models from Planck 2015 and redshift-space distortion data: Andr´e A. Costaa, Xiao-Dong Xub, Bin Wangc, and E. Abdallaa: C.P. 66318, 05315-970, Sa˜o Paulo, SP, Brazil: We investigate phenomenological interactions between dark matter and dark energy and constrain these models by employing the most recent cosmological data including the cosmic microwave background radiation anisotropies from Planck 2015, Type Ia supernovae, baryon acoustic oscillations, the Hubble constant and redshift-space distortions. We ﬁnd that the interaction in the dark sector parameterized as an energy transfer from dark matter to dark energy is strongly suppressed by the whole updated cosmological data. On the other hand, an interaction between dark sectors with the energy ﬂow from dark energy to dark matter is proved in better agreement with the available cosmological observations. This coupling between dark sectors is needed to alleviate the coincidence problem. These data provide the utmost observations on temperature and polarization of the photons from the last scattering surface at redshift around z = 1090. Considering that dark energy and dark matter dominate the energy content of the universe today, it is reasonable to assume that these dark components can interact between themselves. A dark matter and dark energy interaction is an attractive theoretical model, since it can allow solutions with a constant ratio between energy densities of dark matter and dark energy at late times, which can help to alleviate the coincidence problem in the concordance model

a. cosmological b. astrophysical c. relativistic d. dark matter

Q73. Cosmological constraints on Lorentz Invariance violation in gravity and dark matter: Mikhail M., Ivanov FSB/IPHYS/LPPC, Switzerland, Russia: This brief contribution is devoted to phenomenological consequences of deviations from Lorentz invariance in gravity and dark matter. We will discuss main eﬀects on cosmological observables and current constraints derived from astrophysical and cosmological data. Theories without Lorentz invariance provide us with an interesting framework to test modiﬁed gravity models and better understand the role of the Lorentz symmetry. These theories yield peculiar phenomenological eﬀects, which can be examined with cosmological data. The cosmological constraints obtained so far bound LV in gravity at the sub-percent level, and are competitive with those derived from astrophysical test. The bounds on LV in DM were put at the percent level. More studies are required in order to understand the non-linear eﬀects that will allow to test Lorentz invariance to a new level of precision with upcoming,

a. studies b. research c. investigations d. surveys.

Q74. http://arxiv.org/abs/1605.04043: From Extended theories of Gravity to Dark Matter: Sayantan Choudhury, Manibrata Sen, Soumya Sadhukhan: Mumbai. Abstract: we propose diﬀerent models of extended theories of gravity, which are minimally coupled to the SM ﬁelds, to explain the possibility of a dark matter (DM) candidate, without ad-hoc additions to the Standard Model (SM). We modify the gravity sector by allowing quantum corrections motivated from local f(R) gravity, and non-minimally coupled gravity with SM sector and dilaton ﬁeld. Using an eﬀective ﬁeld theory (EFT) framework, we constrain the scale of the EFT and DM mass. We consider two cases-Light DM (LDM) and Heavy DM (HDM), and deduce upper bounds on the DM annihilation cross section to SM,

a. Fields b. Particles c. Bosons d. Fermions.

Q75. http://arxiv.org/abs/1605.04080: Dirac’s Equation in R-Minkowski Space-time: T. Foughali, A. Bouda, Bejaia, Algeria: May 16, 2016: Abstract: We recently constructed the R-Poincar´e algebra from an appropriate deformed Poisson brackets which reproduce the Fock coordinate transformation. We showed then that the space-time of this transformation is the de Sitter one. In this paper, we derive in the R-Minkowski space-time the Dirac equation and show that this is none other than the Dirac equation in the de Sitter space-time given by its conformally ﬂat metric. Furthermore, we propose a new approach for solving Dirac’s equation in the de Sitter space-time using the Schrodinger picture. We constructed the free Dirac equation in the R-Minkowski space-time. After using a certain realization of the R-Poincar´e algebra, it turned out that the obtained equation is exactly the Dirac equation in the conformally ﬂat de Sitter space-time. This is a further proof of the correspondence between the R-Minkowski and the de Sitter space such that the physics of R-Poincar´e algebra is the same as in the de Sitter relativity. So, this correspondence could be used to construct well-deﬁned physical observables in the de Sitter space-time. We also presented a new method for solving Dirac equation in the conformally ﬂat patch of de Sitter space-time within the Schrodinger picture. The latter was introduced by Cot˘aescu to investigate Dirac and Klein-Gordon equations in the context of de Sitter,

a. space b. time c. space-time d. universe.

Q76. Design of a plasmonic near-ﬁeld tip for super-resolution IR-imaging: Fouad Ballout, London, UK: Erik Brundermann, Diedrich A. Schmidt, Martina Havenith, Germany; Abstract: The concepts of spoof surface plasmon polaritons and adiabatic ﬁeld compression are employed to design metallic near-ﬁeld probes that allow guiding and focusing of mid-infrared wavelength electromagnetic radiation and provides subwavelength ﬁeld conﬁnements and a lateral optical resolution of about 10 nm. By means of mode matching, we designed an experimentally feasible surface grating that excites spoof SPPs in the chemical ﬁngerprint region between 5.7 and 6µm (i.e. between 1660 and 1755 cm⁻¹). We grafted this grating onto the surface of a tapered metal waveguide structure to which we appended a nanoscale antenna with a 5nm tip radius. FEM electromagnetic simulations revealed extraordinary ﬁeld enhancement of 2-3 orders higher compared with conventional IR near-ﬁeld probes. This ﬁeld enhancement is accompanied by ﬁeld conﬁnement at the tip apex of the order of 10 nm holding the prospect of a fourfold increase in lateral optical resolution in comparison with conventional metal probes utilized 11 in current s-SNIM apparatus. A goniometric analysis of the ﬁeld excitation revealed a broad range of angles under which extraordinary ﬁeld enhancement can be achieved. Thus, implementation of the nanoprobe presented here into existing near-ﬁeld IR microscopy apparatus should be possible with minor or no modiﬁcations. With such a plasmon-assisted mid-IR nanoscopy probe available the label-free imaging of single protein or lipid molecules within biological tissue is possible. Adapting the grating to the appropriate wavelength, such a probe can be also deployed to detect small ﬂuctuations in the free carrier concentration of highly doped seminconductor

a. nanoscopy b. nanostructures c. nanoprobe d. nanoplasmons.

Q77. Cosmological Constant in the Thermodynamic Models of Gravity: Merab Gogberashvili, Ucha Chutkerashvili, Tbilisi 0177, Georgia: May 16, 2016: Abstract: Within thermodynamic models of gravity, where the universe is considered as a ﬁnite ensemble of quantum particles, cosmological constant in the Einstein’s equations appears as a constant of integration. Then it can be bounded using Karolyhazy uncertainty relation applied for horizon distances, as the amount of information in principle accessible to an external observer. To conclude, in this small note we suggest to identify the cosmological constant, which within the thermodynamic model of gravity appears as a constant of integration, with the amount of information accessible to an external observer. Then its value can be obtained using the Ka´rolyh´azy uncertainty relation applied to the horizon distances, which gives the observed value of the dark energy of

a. fields b. particles c. space-time d. universe

Q78. The connection between Dirac dynamic and parity symmetry: C. H. Coronado Villalobos, R. J. Bueno Rogerio, SP, Brazil. Dirac spinors are important objects in the current literature, the algebraic structure presented in the text-books is a general method to write it, however, not unique. The purpose of the present work is to show an alternative approach to construct Dirac spinors, considering the interchange between the Lorentz representation space (1/2, 0) and (0, 1/2) made by the “Magic of Pauli matrices” and not by parity, as commonly it was thought. As it is well known, parity operator is related with the Dirac dynamics, as it can be seen in the reference of Sperana given below. The major focus is to establish the relation between Dirac dynamics with parity operator, the reverse path shown in L. D. Sperana, An identiﬁcation of the Dirac operator with the Parity operator, Int. Journal of Modern Physics D 2, 1444003 (2014). We are able to obtain four spinors; two of them are dual helicity objects and the remaining two are single helicity objects using the same way of thought used by

a. Elko b. Dirac c. Coronado d. Rogerio

Q79. On the Origin of the XYZ Mesons: A. Valcarce, J. Vijande, Valencia, Spain. Abstract. In this talk we present a mechanism giving rise to exotic XYZ four-quark states in the meson spectra within a constituent quark model approach. We discuss its generalization to ﬁve-quark states in the heavy baryon sector. Finally, we revise some other works in the literature and experimental data where this mechanism may be working. We have presented a plausible mechanism for the origin of the XYZ mesons in the heavy meson spectra within a standard quark-model picture. Its generalization to the heavy baryon sector has been analysed. The existence of open ﬂavour two–hadron thresholds is a feature of the heavy hadron spectra that needs to be considered as a relevant ingredient into any description of the plethora of new states reported in heavy meson and baryon spectroscopy. They might be, at a ﬁrst glance, identiﬁed with simple quark-antiquark or three-quark states, however in some cases their energies and decay properties do not match such oversimpliﬁed picture. Our results prove the relevance of higher or der Fock space components through the allowed two-hadron thresholds. On the one hand, one has the lower (Q ¯ Q)(n¯ n) and (nnn)(Q¯ n) systems, made by almost non-interacting hadrons, that constitutes the natural breaking apart end-state. On the other hand, the higher (Q ¯ n)(n ¯ Q) and (nnQ)(n ¯ n) systems appear. When there is an attractive interaction characterizing the upper systems combined with a strong enough coupling, together with the vicinity of the two allowed thresholds, a multiquark bound state may emerge. As one can see the mechanism proposed is restrictive enough as not predicting a proliferation of bound states when explaining the existence of a hypothetical molecular structure. Once this is performed, the present experimental eﬀort with ongoing experiments at BESIII, current analyses by the LHC collaboration and future experiments at Belle II and Panda together with the very impressive results that are being obtained by lattice gauge theory calculations given in High Energy Phys. 07, 126 (2012) may conﬁrm the theoretical expectations of our quark-model calculation pattern that will provide with a deep understanding of low-energy realizations of QCD.

a. CAM b. ADC c. QMD d. QCD

Q80. Solutions of the Schrodinger equation given by solutions of the Hamilton–Jacobi equation: G.F. Torres del Castillo, C. Sosa-Sanchez, Mexico, May 16, 2016, Abstract: We ﬁnd the form of the potential depending on the coordinates and the time such that a solution, S, of the Hamilton–Jacobi equation yields an exact solution, exp(iS/ћ),of the corresponding Schrodinger equation. The eikonal equation of geometrical optics can be regarded as an approximation to the scalar Helmholtz equation, in a similar manner as the HJ equation is an approximation to the Schrodinger equation and, therefore, one can expect that, in some cases, a solution of the eikonal equation would produce an exact solution of the equation given by

a. Helmholtz b. Schrodinger c. Hamilton-Jacobi d. Eikonal

Q81. Mon. Not. R. Astron. Soc. 000, 1–19 (2013): 20 May 2016. A ram-pressure threshold for star formation: A. P. Whitworth, Cardiﬀ CF24 3AA, Wales, UK. ABSTRACT: In turbulent fragmentation, star formation occurs in condensations created by converging ﬂows. The condensations must be suﬃciently massive, dense and cool to be gravitationally unstable, so that they start to contract; and they must then radiate away thermal energy fast enough for self-gravity to remain dominant, so that they continue to contract. For the metallicities and temperatures in local star forming clouds, this second requirement is only met robustly when the gas couples thermally to the dust, because this delivers the capacity to radiate across the full bandwidth of the continuum, rather than just in a few discrete spectral lines. This translates into a threshold for vigorous star formation, which can be written as a minimum ram-pressure PCRIT ∼ 4×10^-11 dyne. PCRIT is independent of temperature, and corresponds to ﬂows with molecular hydrogen number-density n _H2.FLOW and velocity v FLOW satisfying n_H2.FLOW *v^2 FLOW > ∼ 800cm⁻³(km/s)². This in turn corresponds to a minimum molecular hydrogen column-density for vigorous star formation, N _H2.CRIT ∼ 4×10²¹cm⁻² (Σ_CRIT ∼ 100M_⊙pc⁻²), and a minimum visual extinction A_V,CRIT ∼ 9mag. The characteristic diameter and line-density for a star-forming ﬁlament when this threshold is just exceeded – a sweet spot for local star formation regions – are 2R_FIL ∼ 0.1pc and µ_FIL ∼ 13M_⊙pc⁻². The characteristic diameter and mass for a pre-stellar core condensing out of such a ﬁlament are 2R_CORE ∼ 0.1pc, and M_CORE ∼ 1M_⊙. We also show that fragmentation of a shock-compressed layer is likely to commence while the convergent ﬂows creating the layer are still ongoing, and we stress that, under this circumstance, the phenomenology and characteristic scales for fragmentation of the layer are fundamentally diﬀerent from those derived traditionally for pre-existing

a. characteristics b. scales c. layers d. stress.

Q83. Astronomy & Astrophysics manuscript no. a47 c, ESO 2016, May 20, 2016. Optical spectroscopy of Be/gamma-ray binaries: R. K. Zamanov, K. A. Stoyanov, J. Martí, G. Y. Latev, Y. M. Nikolov, M. F. Bode, and P. L. Luque-Escamilla, Spain: ABSTRACT: We report optical spectroscopic observations of the γ-ray binaries LSI+61⁰ 303, MWC 656, MWC 148. The peak separation and equivalent widths of prominent emission lines (H_α, H_β, Hγ, He-I and Fe-II) are measured. We estimate the circumstellar disc size, compare it with separation between the components and discuss the disc truncation. We ﬁnd that in LSI+610303 the compact object comes into contact with the outer parts of the circumstellar disc at periastron; in MWC 148 the compact object goes deeply into the disc during the periastron passage, and in MWC 656 the black hole is accreting from the outer parts of the circumstellar disc along the entire orbit. The interstellar extinction is estimated using interstellar lines and hydrogen column density. The rotation of the mass donors appears to be similar to the rotation of the mass donors in Be/X-ray binaries. We suggest that X-ray periodicity ∼1 day deserves to be searched for. The main results of our spectroscopic observations of LSI+610303, MWC 148 and MWC 656 are, 1. The histograms in all three stars show that the disc size clusters at speciﬁc levels, indicating the circumstellar disc is truncated by the orbiting compact object. 2. In LSI+610303 the neutron star crosses the outer parts of the circumstellar disc at periastron; in MWC 148 the compact object passes deeply through the disc during the periastron passage, and in MWC 656 the black hole is accreting from the outer parts of the circumstellar disc during the entire orbital cycle. 3. We estimate the interstellar extinction towards LSI+610303, MWC 148 and MWC 656. The rotation of the mass donors is similar to that of the Be/X-ray binaries. We suggest that the three stars deserve to be searched for an X-ray periodicity of about 1.0 day.

a. 1 day b. 100 days c. 10 days d. 3 days.

Q84. MNRAS 000, 1–14 (2016): Preprint 27 May 2016: An ultra-dense fast out ﬂow in a quasar at z=2.4: R. J. Williams, R. Maiolino, Y. Krongold, S. Carniani, G. Cresci, F. Mannucci, A. Marconi: Cavendish Laboratory, University of Cambridge, 19 J.J. Thomson Ave., Cambridge etc., ABSTRACT We present Adaptive Optics assisted near-IR integral ﬁeld spectroscopic observations of a luminous quasar at z = 2.4, previously observed as the ﬁrst known example at high redshift of large scale quasar-driven outﬂow quenching star formation in its host galaxy. The nuclear spectrum shows broad and blue shifted Hβ in absorption, which is tracing out ﬂowing gas with high densities (> 108 – 109 cm⁻³) and velocities in excess of 10,000 km s⁻¹. The properties of the outﬂowing clouds (covering factor, density, column density and inferred location) indicate that they likely originate from the Broad Line Region. The energetics of such nuclear regions are consistent with that observed in the large scale outﬂow, supporting models in which quasar driven outﬂows originate from the nuclear region and are energy conserving. We note that the asymmetric proﬁle of both the Hβ and Hα emission lines is likely due to absorption by the dense outﬂowing gas along the line of sight. This outﬂow-induced asymmetry has implications on the estimation of the black hole mass using virial estimators, and warns about such effects for several other quasars characterized by similar line asymmetries. More generally, our ﬁndings may suggest a broader revision of the decomposition and interpretation of quasar spectral features, in order to take into account the presence of potential broad blue shifted Balmer absorption lines. Our high spatial resolution data also reveals redshifted, dynamically colder nebular emission lines, likely tracing an inﬂowing stream. We also note that the absorption of the blue side of the Balmer lines due to such dense outﬂowing gas has a signiﬁcant impact on the determination of black hole masses based on virial estimators, prompting for a revision of the black hole masses in quasars with,

a. asymmetric lines b. broad lines c. symmetric lines d. distorted lines

Q85. Mon. Not. R. Astron. Soc. 000, 1–11, 27 May 2016: Acceleration of the universe: a reconstruction of the eﬀective equation of state: Ankan Mukherjee, Kolkata, Mohanpur, West Bengal-741246, India: ABSTRACT: The present work is based upon a parametric reconstruction of the eﬀective or total equation of state in a model for the universe with accelerated expansion. The constraints on the model parameters are obtained by maximum likelihood analysis using the supernova distance modulus data, observational Hubble data, baryon acoustic oscillation data and cosmic microwave background shift parameter data. For statistical comparison, the same analysis has also been carried out for the wCDM dark energy model. Diﬀerent model selection criteria (Akaike information criterion (AIC)) and (Bayesian Information Criterion (BIC)) give the clear indication that the reconstructed model is well consistent with the wCDM model. Then both the models (Weff(z) model and wCDM model) have also been presented through (q₀ , j₀) parameter space. Tighter constraint on the present values of dark energy equation of state parameter (wDE (z = 0)) and cosmological jerk (j₀) have been achieved for the reconstructed model.

a. state b. model c. parameter d. constraint.

Q86. MNRAS 000, 1–10 (2016) Preprint 27 May 2016: LOTUS: A low cost, ultraviolet spectrograph: I. A. Steele, J. M. Marchant, H. E. Jermak, R. M. Barnsley, S .D. Bates, N.R. Clay, A. Fitzsimmons, E. Jehin, G. Jones, C. J. Mottram, R. J. Smith, C. Snodgrass, M. de Val-Borro, ect., Department of Astrophysical Sciences, Princeton University, NJ 08544, USA: Accepted 2016 May 26. Received 2016 May 26; in original form 2015 December 10: ABSTRACT: We describe the design, construction and commissioning of LOTUS; a simple, low-cost long-slit spectrograph for the Liverpool Telescope. The design is optimized for near-UV and visible wavelengths and uses all transmitting optics. It exploits the instrument focal plane ﬁeld curvature to partially correct axial chromatic aberration. A stepped slit provides narrow (2.5 × 95 arcsec) and wide (5 × 25 arcsec) options that are optimized for spectral resolution and ﬂux calibration respectively. On sky testing shows a wavelength range of 3200–6300 ˚A with a peak system throughput (including detector quantum eﬃciency) of 15 per cent and wavelength dependant spectral resolution of R = 225−430. By repeated observations of the symbiotic emission line star AG Peg we demonstrate the wavelength stability of the system is < 2 ˚A rms and is limited by the positioning of the object in the slit. The spectrograph is now in routine operation monitoring the activity of comet 67P/Churyumov-Gerasimenko during its current post-perihelion,

a. operation b. partition c. apparition d. positioning.

Q87. May 26, 2016: Enabling science with Gaia observations of naked-eye stars: J. Sahlmann, J. Mart´ın-Fleitasb, A. Morab, A. Abreub, C. M. Crowleyb, E. Jolietb, European Space Agency, STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA; etc. ABSTRACT ESA’s Gaia space astrometry mission is performing an all-sky survey of stellar objects. At the beginning of the nominal mission in July 2014, an operation scheme was adopted that enabled Gaia to routinely acquire observations of all stars brighter than the original limit of G∼6, i.e. the naked-eye stars. Here, we describe the current status and extent of those observations and their on-ground processing. We present an overview of the data products generated for G<6 stars and the potential scientiﬁc applications. Finally, we discuss how the Gaia survey could be enhanced by further exploiting the techniques we developed. There are about 6000 stars that can be observed with the unaided human eye. (1) Make the community aware of the data products that potentially will be made available as part of a Gaia data release. (2) Identify areas where ancillary observations collected by independent observers and observatories contemporaneously with Gaia can signiﬁcantly enhance the scientiﬁc output. (3) Provide scientiﬁc motivation to pursue and enhance the acquisition and analysis of very bright star data.

a. Data b. sources c. positions d. observations

Q88. Prog. Theor. Exp. Phys. 2015, (9 pages):Thermodynamic properties of black holes in de Sitter space: Huai-Fan Li, Meng-Sen Ma, and Ya-Qin Ma: Datong 037009, China: etc., ABSTRACT: We study the thermodynamic properties of Schwarzschild-de Sitter (SdS) black hole and Reissner-Nordstro¨m-de Sitter (RNdS) black hole in the view of global and eﬀective thermodynamic quantities. Making use of the eﬀective ﬁrst law of thermodynamics, we can derive the eﬀective thermodynamic quantities of de Sitter black holes. It is found that these eﬀective thermodynamic quantities also satisfy Smarr-like formula. Especially, the eﬀective temperatures are nonzero in the Nariai limit, which is consistent with the idea of Bousso and Hawking. By calculating heat capacity and Gibbs free energy, we ﬁnd SdS black hole is always thermodynamically stable and RNdS black hole may undergoes phase transition at some points.

a. spaces b. rounds c. gaps d. points.

Q89. 26 May 2016: Spin Gravitational Resonance and Graviton Detection: James Q. Quach∗ Institute for Solid State Physics, University of Tokyo, Kashiwa, Chiba 277-8581, Japan: ABSTRACT: We develop a gravitational analogue of spin magnetic resonance, called spin gravitational resonance, whereby a gravitational wave interacts with a magnetic ﬁeld to produce a spin transition. In particular, an external magnetic ﬁeld separates the energy spin states of a spin-1/2 particle, and the presence of the gravitational wave produces a perturbation in the components of the magnetic ﬁeld orthogonal to the gravitational wave propagation. In this framework we test Dyson’s conjecture that individual gravitons cannot be detected. Although we ﬁnd no fundamental laws preventing single gravitons being detected with spin gravitational resonance, we show that it cannot be used in practice, in support of Dyson’s

a. proposition b. idea c. conjecture d. postulate

Q90. MNRAS in press, 1–20 (2016) Preprint 22 June 2016: Precise limits on cosmological variability of the ﬁne-structure constant with zinc and chromium quasar absorption lines: Michael T. Murphy, Adrian L. Malec, J. Xavier Prochaska; Santa Cruz, CA 95064, USA.16 June 2016: ABSTRACT: The strongest transitions of Zn and CrII are the most sensitive to relative variations in the ﬁne-structure constant (∆α/α) among the transitions commonly observed in quasar absorption spectra. They also lie within just 40˚A of each other (rest frame), so they are resistant to the main systematic error aﬀecting most previous measurements of ∆α/α: long-range distortions of the wavelength calibration. While Zn and CrII absorption is normally very weak in quasar spectra, we obtained high signal-to-noise, high-resolution echelle spectra from the Keck and Very Large Telescopes of 9 rare systems where it is strong enough to constrain ∆α/α from these species alone. These provide 12 independent measurements (3 quasars were observed with both telescopes) at redshifts 1.0–2.4, 11 of which pass stringent reliability criteria. These 11 are all consistent with ∆α/α = 0 within their individual uncertainties of 3.5–13parts per million (ppm), with a weighted mean ∆α/α = 0.4±1.4stat ±0.9sys ppm (1σ statistical and systematic uncertainties), indicating no signiﬁcant cosmological variations in α. This is the ﬁrst statistical sample of absorbers that is resistant to long-range calibration distortions (at the <1ppm level), with a precision comparable to previous large samples of ∼150 (distortion-aﬀected) absorbers. Our systematic error budget is instead dominated by much shorter-range distortions repeated across echelle orders of individual

a. spectrums b. spectra c. orders d. disorders

Q91. Monthly Notices of the Royal Astronomical Society, 2016 MAY 20; REVISED 2016, JUNE 16: A QUINTUPLE STAR SYSTEM CONTAINING TWO ECLIPSING BINARIES S. RAPPAPORT1, H. LEHMANN2, B. KALOMENI1, T. BORKOVITS, D. LATHAM5, A. BIERYLA, H. NGO, D. MAWET, S. HOWELL, E. HORCH T. L. JACOBS, D. LACOURSE, Á. SÓDOR, A. VANDERBURG5, K. PAVLOVSKI: ABSTRACT: We present a quintuple star system that contains two eclipsing binaries. The unusual architecture includes two stellar images separated by 1100 on the sky: EPIC 212651213 and EPIC 212651234. The more easterly image (212651213) actually hosts both eclipsing binaries which are resolved within that image at 0.0900, while the westerly image (212651234) appears to be single in adaptive optics (AO), speckle imaging, and radial velocity (RV) studies. The ‘A’ binary is circular with a 5.1-day period, while the ‘B’ binary is eccentric with a 13.1-day period. The γ velocities of the A and B binaries are different by∼10 km s−1. That, coupled with their resolved projected separation of 0.0900, indicates that the orbital period and separation of the ‘C’ binary (consisting of A orbiting B) are '65 years and '25 AU, respectively, under the simplifying assumption of a circular orbit. Motion within the C orbit should be discernible via future RV, AO, and speckle imaging studies within a couple of years. The C system (i.e., 212651213) has a radial velocity and proper motion that differ from that of 212651234 by only∼1.4 km s−1 and∼3 mas yr−1. This set of similar space velocities in 3 dimensions strongly implies that these two objects are also physically bound, making this at least a quintuple

a. Star system b. binary system c. mass system d. quadrupole

Q92. June 20, 2016:[gr-qc]:arXiv1606:066331v!: Electrodynamics of a Cosmic Dark Fluid: Alexander B. Balakin, Kazan, Russia: ABSTRACT: Cosmic Dark Fluid is considered as a non-stationary medium, in which electromagnetic waves propagate, and magneto-electric ﬁeld structures emerge and evolve. A medium type of representation of the Dark Fluid allows us to involve into analysis the concepts and mathematical formalism elaborated in the framework of classical covariant electrodynamics of continua, and to distinguish dark analogues of well-known medium-eﬀects, such as optical activity, pyro-electricity, piezo-magnetism, electro and magneto-striction and dynamo-optical activity. The Dark Fluid is assumed to be formed by a duet of a Dark Matter (a pseudoscalar axionic constituent) and Dark Energy (a scalar element); respectively, we distinguish electrodynamic eﬀects induced by these two constituents of the Dark Fluid. The review contains discussions of ten models, which describe electrodynamic eﬀects induced by Dark Matter and/or Dark Energy. The models are accompanied by examples of exact solutions to the master equations, correspondingly extended; applications are considered for cosmology and space-times with spherical and pp-wave symmetries. In these applications we focused the attention on three main electromagnetic phenomena induced by the Dark Fluid: ﬁrst, emergence of Longitudinal Magneto-Electric Clusters; second, generation of anomalous electromagnetic responses; third, formation of Dark Epochs in the Universe history.

a. Energy b. Spectrum c. History d. clusters.

Q93. arXiv:19 June 2016: [gr-qc]: On a phenomenology of the accelerated expansion with a varying ghost dark energy: M. Zh. Khurshudyana, A. N. Makarenkob, Russian Federation: June 22, 2016: Abstract: Subject of our study it is the accelerated expansion of the large scale universe, where a varying ghost dark energy can take the role of the dark energy. The model of the varying ghost dark energy considered in this work it is a phenomenological modiﬁcation of the ghost dark energy. Recently, three other phenomenological models of the varying ghost dark energy have been suggested and the model considered in this work will complete the logical chain of considered modiﬁcations. The best ﬁt of theoretical results to the luminosity distance, has been used to obtain preliminary constraints on the parameters of the models. This does help us to reduce amount of discussion. On the other hand, detailed comparison of theoretical results with observational data has been left as a subject of another discussion elsewhere. Moreover, a look to considered models via Om and state ﬁnder hierarchy analysis is presented and discussed for diﬀerent forms of interaction between the varying ghost dark energy and cold dark,

a. space b. energy c. ghost d. matter

Q94. MITP/16-055: Mass, zero mass and … nophysics: R. Saar and S. Groote, Mainz, Germany; Abstract: In this paper we demonstrate that massless particles cannot be considered as limiting case of massive particles. Instead, the usual symmetry structure based on semisimple groups like U(1), SU(2) and SU(3) has to be replaced by less usual solvable groups like the minimal nonabelian group sol2. Starting from the proper orthochronous Lorentz group Lor1,3 we extend Wigner’s little group by an additional generator, obtaining the maximal solvable or Borel subgroup Bor1,3 which is equivalent to the Kronecker sum of two copies of sol2, telling something about the helicity of particle and antiparticle

a. legends b. nophysics c. states d. Groups.

Q95. Astronomy & Astrophysics ESO 2016 June 23, 2016: The global distribution of magnetic helicity in the solar corona: A. R. Yeates and G. Hornig::anthony.yeates@durham.ac.uk, DD1 4HN, UK: ABSTRACT: By deﬁning an appropriate ﬁeld line helicity, we apply the powerful concept of magnetic helicity to the problem of global magnetic ﬁeld evolution in the Sun’s corona. As an ideal-magnetohydrodynamic invariant, the ﬁeld line helicity is a meaningful measure of how magnetic helicity is distributed within the coronal volume. It may be interpreted, for each magnetic ﬁeld line, as a magnetic ﬂux linking with that ﬁeld line. Using magneto-frictional simulations, we investigate how ﬁeld line helicity evolves in the non-potential corona as a result of shearing by large-scale motions on the solar surface. On open magnetic ﬁeld lines, the helicity injected by the Sun is largely output to the solar wind, provided that the coronal relaxation is suﬃciently fast. But on closed magnetic ﬁeld lines, helicity is able to build up. We ﬁnd that the ﬁeld line helicity is non-uniformly distributed, and is highly concentrated in twisted magnetic ﬂux ropes. Eruption of these ﬂux ropes is shown to lead to sudden bursts of helicity output, in contrast to the steady ﬂux along the open magnetic ﬁeld,

a. shapes b. lines c. helicity d. non-uniformity

Q96. Elementary quantum mechanics of the neutron with an electric dipole moment; Gordon Bayma and D. H. Beck; Urbana, IL 61801 (Dated: June 23, 2016): The neutron, in addition to possibly having a permanent electric dipole moment as a consequence of violation of time-reversal invariance, develops an induced electric dipole moment in the presence of an external electric ﬁeld. We present here a uniﬁed non-relativistic description of these two phenomena, in which the dipole moment operator, ~ D, is not constrained to lie along the spin operator. Although the expectation value of ~ D in the neutron is less than 10⁻¹³ of the neutron radius, r_n the expectation value of ~ D² is of order r²_n. We determine the spin motion in external electric and magnetic ﬁelds, as employed in past and future searches for a permanent dipole moment, and show that the neutron electric polarizability, although entering the neutron energy in an external electric ﬁeld, does not aﬀect the spin motion. In a simple non-relativistic model we show that the expectation value of the permanent dipole is, to lowest order, proportional to the product of the time reversal-violating coupling strength and the electric polarizability of the neutron. we have related the permanent dipole moment of the neutron to an admixture of a component of the neutron wave function with opposite parity and time-reversal symmetry, and shown that the electric polarizability of the neutron involves a similar admixture, but with opposite time-reversal symmetry, in the wave function. In the absence of external ﬁelds, the expectation value of the electric dipole moment lies in the direction of the expectation value of the spin; in an applied electric ﬁeld the induced moment is parallel to the ﬁeld. Although the energy of the neutron in an electric ﬁeld depends on its polarizability, the precession of the spin in external electric and magnetic ﬁelds is independent of the polarizability. We have also examined a simple model of the source of the CP-violating component of the particle wave function, showing that there is an approximate cancellation of structure eﬀects in the ratio of the permanent moment and the polarizability. Such structure eﬀects remain important in interpreting future experiments in terms of fundamental interactions.

a. forces b. interactions c. terms d. constants

Q97. Spin- and valley-polarized transport across line defects in monolayer MoS₂: Artem Pulkin and Oleg V. Yazyev, Switzerland (Dated: June 23, 2016). We address the ballistic transmission of charge carriers across ordered line defects in monolayer transition metal dichalcogenides. Our study reveals the presence of a transport gap driven by spin-orbit interactions, spin and valley ﬁltering, both stemming from a simple picture of spin and momentum conservation, as well as the electron-hole asymmetry of charge-carrier transmission. Electronic transport properties of experimentally observed ordered line defects in monolayer MoS₂, in particular, the vacancy lines and inversion domain boundaries, are further investigated using ﬁrst principles Green’s function methodology. Our calculations demonstrate the possibility of achieving nearly complete spin polarization of charge carriers in nano-electronic devices based on engineered periodic line defects in monolayer transition metal dichalcogenides, thus suggesting a practical scheme for all-electric control of spin transport. Our work reveals a number of transport phenomena in the transmission of charge carriers across ordered line defects in monolayer MoS2 stemming from a simple and intuitive picture of spin and momentum conservation combined with strong spin-orbit eﬀects in this two-dimensional material.

a. material b. orbits c. charges d. devices

Q98. [Cs.LG] 22 June 2016; arXiv: 1606.07035V1: Ancestral Causal Inference: Sara Magliacane VU; s.magliacane@uva.nl : Tom Claassen; tomc@cs.ru.nl; Joris M. Mooij: j.m.mooij@uva.nl : Abstract: Constraint-based causal discovery from limited data is a notoriously difﬁcult challenge due to the many borderline independence test decisions. Several approaches to improve the reliability of the predictions by exploiting redundancy in the independence information have been proposed recently. Though promising, existing approaches can still be greatly improved in terms of accuracy and scalability. We present an method that reduces the combinatorial explosion of these arch-space by using a more coarse-grained representation of causal information, drastically reducing computation time. Additionally, we propose a method to score causal predictions based on their conﬁdence. Crucially, our implementation also allows one to easily combine observational and interventional data and to incorporate various types of available background knowledge. We prove soundness and asymptotic consistency of our method and demonstrate that it can outperform the state-of the-art on synthetic data, achieving a speedup of several orders of magnitude. We illustrate its practical feasibility by applying it on a challenging protein data set. As illustrated by our example, in real-world experiments ﬁnding cause-effect relations is paramount, and ancestral structures are very well-suited to that end. They also offer a natural way to incorporate background causal knowledge, e.g., from other experiments. On top of that, in the context of algorithms that aim for error-correction by exploiting redundant information, they also allow a huge computational advantage over existing edge-based representations. When needed, the ancestral structures are easily mapped to a more ﬁne-grained structural representation to indicate direct and indirect causal relations, using the skeleton implied by the output independence weights. Providing conﬁdence estimates on causal predictions is extremely helpful in practice, and can signiﬁcantly boost reliability of the output as perceived by researchers. Although standard methods to do so, like bootstrapping (C)FCI, already provide reasonable estimates, having a global optimization method that take into account all conﬁdences in the input causal and independence statements is likely to lead to further improvements of the reliability of causal relations inferred from data. Strangely (or fortunately) enough, neither of the global optimization methods seems to improve much with higher order independence test results. In other words: both already obtain near optimal error-correction behaviour just exploiting up to order-1 independences. We conjecture that this may happen because our loss function essentially assumes that the test results are independent from another (which is not true). Finding a way to take this into account in the loss function may further improve the achievable accuracy, but at the moment the exact relationship between test results is still unclear. Finally, we plan to explore the possibility of extending our ancestral approach to much larger models by incorporating it as a modular routine in a large-scale causal discovery

a. mode b. route c. assertion d. method.

Q99. Stochastic Runge–Kutta Software Package for Stochastic Differential Equations: M. N. Gevorkyan,T. R. Velieva, A. V. Korolkova, D. S. Kulyabov, and L. A. Sevastyanov: Russia: As a result of the application of a technique of multistep processes stochastic models construction the range of models, implemented as a self-consistent differential equations, was obtained. These are partial differential equations (master equation, the Fokker–Planck equation) and stochastic differential equations (Langevin equation). However, analytical methods do not always allow to research these equations adequately. It is proposed to use the combined analytical and numerical approach studying these equations. For this purpose the numerical part is realized within the framework of symbolic computation. It is recommended to apply stochastic Runge–Kutta methods for numerical study of stochastic differential equations in the form of the Langevin. Under this approach, a program complex on the basis of analytical calculations metasystem Sage is developed. For model verification logarithmic walks and Black–Scholes two-dimensional model are used. To illustrate the stochastic “predator–prey” type model is used. The utility of the combined numerical-analytical approach is demonstrated. Some realizations of stochastic Runge-Kutta methods were considered in this article. The authors gradually developed and refined the library by adding a new functionalities and optimizing existing ones. To date, the library uses numerical methods by the Ro¨ßler’s article [9], as the most effective of the currently known to the authors. However, the basic functions strongSRKW1 and weakSRKp2Wm are written in accordance with the general algorithm and can use any Butcher table with appropriate staging. This allows any user of the library to extend functionality by adding new methods. Additional examples of library usage and of all files source codes are available at https://bitbucket.org/mngev/ sde-numerical-integrators. The authors supposed to maintain the library by adding new

a. methods b. functions c. tricks d. algorithms

Q100. MNRAS 000, 1–7 (2016): The X-ray Pulsar M82 X-2 on its Propeller Line: D. M. Christodoulou, D. Kazanas, S. G. T. Laycock; MA, 01854, USA; 24 June 2016: ABSTRACT: NuSTAR has detected pulsations from the ultra-luminous X-ray source X-2 in M82 and archival Chandra observations have given us a good idea of its duty cycle. The newly discovered pulsar exhibited at least 4 super-Eddington outbursts in the past 15 years but, in its lowest-power state, it radiates just below the Eddington limit and its properties appear to be typical of high-mass X-ray binaries. M82 X-2 has been described as a common neutron star with a 1 TG magnetic ﬁeld that occasionally accretes above the Eddington rate and as a magnetar-like pulsar with a 10-100 TG magnetic ﬁeld that reaches above the quantum limit. We argue in favour of the former interpretation. Using standard accretion theory and the available observations, we calculate the stellar magnetic ﬁeld of this pulsar in two independent ways and we show that it cannot exceed 3 TG in either case. We discuss the implications of our results for other ultra-luminous X-ray sources that occasionally exhibit similar powerful

a. Out-fills b. emissions c. out-bursts d. absorptions

Q101. Boron Abundances Across the “Li-Be Dip” in the Hyades Cluster: Ann Merchant Boesgaard, Michael G. Lum, boes@ifa.hawaii.edu; mikelum@ifa.hawaii.edu; Constantine P. Deliyannis, cdeliyan@indiana.edu; Jeremy R. King; jking2@clemson.edu; Marc H. Pinsonneault, & Garrett Somers, pinsonneault.1@osu.edu; ABSTRACT: Dramatic deﬁciencies of Li in the mid-F dwarf stars of the Hyades cluster were discovered by Boesgaard & Tripicco. Boesgaard & King discovered corresponding, but smaller, deﬁciencies in Be in the same narrow temperature region in the Hyades. With the Space Telescope Imaging Spectrograph on the Hubble Space Telescope we investigate B abundances in the Hyades F stars to look for a potential B dip using the B I resonance line at 2496.8 ˚A. The light elements, Li, Be, and B, are destroyed inside stars at increasingly hotter temperatures: 2.5, 3.5, and 5×10⁶ K respectively. Consequently, these elements survive to increasingly greater depths in a star and their surface abundances indicate the depth and thoroughness of mixing in the star. We have (re)determined Li abundances/upper limits for 79 Hyades dwarfs, Be for 43 stars, and B in ﬁve stars. We ﬁnd evidence for a small drop in the B abundance across the Li-Be dip. The B abundances for the four stars in the temperature range 6100 - 6730 K ﬁt the B-Be correlation found previously by Boesgaard et al. Models of rotational mixing produce good agreement with the relative depletions of Be and B in the dip region. We have compared our nLTE B abundances for the three high B stars on either side of the Li-Be dip with those found by Duncan et al. for the two Hyades giants. This conﬁrms the factor of 10 decline in the B abundance in the Hyades giants as predicted by dilution due to the deepening of the surface convection

a. surfaces b. tilts c. elements d. zone.

Q102. arXiv:1606.07184v1 [q-bio.OT] 23 Jun 2016: The “Hard Problem” of Life: Sara Imari Walker and Paul C.W. Davies; sara.i.walker@asu.edu; There are few open problems in science as perplexing as the nature of life and consciousness. At present, we do not have many scientiﬁc windows into either. In the case of consciousness, it seems evident that certain aspects will ultimately defy reductionist explanation, the most important being the phenomenon of qualia, roughly speaking our subjective experience as observers. It is a priori far from obvious why we should have experiences such as the sensation of the smell of coﬀee or the blueness of the sky. Subjective experience isn’t necessary for the evolution of intelligence (we could for example be zombies in the philosophical sense and appear to function just as well from the outside with nothing going on inside). Even if we do succeed in eventually uncovering a complete mechanistic understanding of the wiring and ﬁring of every neuron in the brain, it might tell us nothing about thoughts, feelings and what it is like to experience something. Our phenomenal experiences are the only aspect of consciousness that appears as though it cannot, even in principle, be reduced to known physical principles. This led Chalmers to identify pinpointing an explanation for our subjective experience as the “hard problem of consciousness” [5]. The corresponding “easy problems” (in practice not so easy) are associated with mapping the neural correlates of various experiences. By focusing attention on the problem of subjective experience, Chalmers highlighted the truly inexplicable aspect of consciousness, based on our current understanding. The issue however is by no means conﬁned to philosophy. Chalmers own proposed resolution is to regard subjective consciousness as an irreducible, fundamental property of mind, with its own laws and principles. Progress can be expected to be made by focusing on what would be required for a theory of consciousness to stand alongside our theories for matter, even if it turns out that something fundamentally new is not necessary. The same may be true for life. With the case of life, it seems as though we have a better chance of understanding it as a physical phenomenon than we do with consciousness. It may be the case that new principles and laws will turn out to be unnecessary to explain life, but meanwhile their pursuit may bring new insights to the problem [6]. Some basic aspects of terrestrial biology, for example, replication, metabolism and compartmentalization, can almost certainly be adequately explained in terms of known principles of physics and chemistry, and so we deem explanations for these features to belong to the “easy problem” of life. Research on life’s origin for the past century, since the time of Oparin and Haldane and the “prebiotic soup” hypothesis, has focused on the easy problem, albeit with limited progress. The more pressing question of course is whether all properties of life can in principle be brought under the “easy” category, and accounted for in terms of known physics and chemistry, or whether certain aspects of living matter will require something fundamentally new. This is especially critical in astrobiology, without an understanding of what is meant by “life” we can have little hope of solving the problem of its origin or to provide a general-purpose set of criteria for identifying it on other worlds. As a ﬁrst step in addressing this issue we need to clarify what is meant by the “hard problem” of life; that is, to identify which aspects of biology are likely to prove refractory in attempts to reduce them to known physics and chemistry, in the same way that Chalmers identiﬁed qualia as central to the hard problem of consciousness. To that end we propose that the hard problem of life is the problem of how ‘information’ can aﬀect the world. In this essay we motivate both why the problem of information is central to explaining life and why it is hard, that is, why we suspect that a full resolution of the hard problem will not ultimately be reducible to known physical

a. thoughts b. theorems c. principles d. rules.

Q103. DropNeuron: Simplifying the Structure of Deep NeuralNetworks: WeiPan; w.pan11@imperial.ac.uk; HaoDong; hd311@imperial.ac.uk; YikeGuo; y.guo@imperial.ac.uk; Abstract: Deep learning using multi-layer neural networks (NNs) architecture manifests superb power in modern machine learning systems. The trained Deep Neural Networks (DNNs) are typically large. The question we would like to address is whether it is possible to simplify the NN during training process to achieve a reasonable performance within an acceptable computational time. We presented a novel approach of optimising a deep neural network through regularisation of network architecture. We proposed regularisers which support a simple mechanism of dropping neurons during a network training process. The method supports the construction of a simpler deep neural networks with compatible performance with its simpliﬁed version. As a proof of concept, we evaluate the proposed method with examples including sparse linear regression, deep auto-encoder and convolutional neural network. The valuations demonstrate excellent performance. We presented a novel approach of optimising a deep neural network through regularisation of network architecture. We proposed regularises which support a simple mechanism of dropping neurons during a network training process. The method supports the construction of a simpler deep neural networks with compatible performance with its simpliﬁed version. We evaluate the proposed method with few examples including sparse linear regression, deep auto-encoding and convolutional net. The valuations demonstrate excellent performance. This research is in its early stage. First, we have noticed that for speciﬁc deep NN structures such as Convolutional NN, Recurrent NN, Restricted Boltzmann Machine, etc, the regularises need to be adjusted respectively. Second, we also notice that Dropout training in deep NN as approximate Bayesian inference in deep Gaussian processes which offer a mathematically grounded framework to reason about model uncertainty. Both l0 regularise and l1 regulariser may be potentially explained from Bayesian perspective by introducing speciﬁc kernel

a. functions b. regulars c. derivatives d. valuations

Q104. ABSTRACT: The Physics of Bioﬁlms: An Introduction Marco G. Mazza∗ Max Planck Institute for Dynamics and Self-Organization, Am Faßberg 17, 37077 Göttingen, Germany (Dated: June 7, 2016)arXiv:1606.01392v1 [physics.bio-ph] 4 June 2016; Bioﬁlms are complex, self-organized consortia of microorganisms that produce a functional, protective matrix of biomolecules. Physically, the structure of a bioﬁlm can be described as an entangled polymer network which grows and changes under the eﬀect of gradients of nutrients, cell diﬀerentiation, quorum sensing, bacterial motion, and interaction with the environment. Its development is complex, and constantly adapting to environmental stimuli. Here, we review the fundamental physical processes that govern the inception, growth and development of a bioﬁlm. Two important mechanisms guide the initial phase in a bioﬁlm life cycle: (i) the cell motility near or at a solid interface, and (ii) the cellular adhesion. Both processes are crucial for initiating the colony and for ensuring its stability. A mature bioﬁlm behaves as a viscoelastic ﬂuid with a complex, history-dependent dynamics. We discuss progress and challenges in the determination of its physical properties. Experimental and theoretical methods are now available that aim at integrating the bioﬁlm’s hierarchy of interactions, and the heterogeneity of composition and spatial structures. We also discuss important directions in which future work should be directed. We have reviewed the theoretical and computational modelling of bioﬁlms. Computational approaches at simulating a bioﬁlm are now ﬁnally coming of age, and some predictions quantitatively match the experimental data, but much remains to be done. Ahead lies a particularly daunting challenge when considering all the chemical, biological and physical processes involved in a bioﬁlm, which evolve and interact from the nano-meter to the milli-meter length scale, and from the nanosecond time scale to hours or days. Future lines of development should include realistic models for the EPS, either microscopically with a polymer network theory, or mesoscopically with a viscoelastic model. Some attempts are already available, where the bioﬁlm is modelled with breakable springs in an immersed boundary method, or through a nonlinear, continuum description of worm-like chains. Once integrated theoretical and computational models will be developed, they will allow to test and manipulate bioﬁlms under multiple physical, chemical and biological cues, both intrinsic and extrinsic. We now want to enter a more speculative realm to discuss some mechanisms at play in the bioﬁlm that could be recognized in the future. The important fact that bioﬁlms represent the most complex eﬀort of simple microorganisms at multicellular organization points to the existence of ‘communications’ channels among the individual cells. We know from the biology of multicellular eukaryotes how a complex, well-regulated and specialized structure may exist. Bioﬁlms are more dynamical and history-dependent in their structure and properties. However, interactions that lead to specialization must be there also in bioﬁlms. Obvious candidates are quorum sensing and cell signalling. Although the role of quorum sensing has been linked multiple times with the growth, structure and function of bioﬁlms, controversial results abound. The reason for the controversy is probably the inadequacy of our experimental tools of investigation to the task: more subtle tools for in vivo and in situ analysis are required; another factor that complicates the picture is that the study of mutants elicits the risk of pleiotropy. We speculate that quorum sensing and cell signalling provide the communication channels required to generate complex organization. A second physical aspect that is underrepresented in the study of bioﬁlms is the role of motility. We have reviewed the available evidence on the function of swimming, swarming and twitching within a bioﬁlm. We speculate, however, that these motility modes should have a more important role than currently known. While under some physical forces, such as hydrodynamic shear, a bioﬁlm might respond by forming more compact structures with asessile population, consortia of diﬀerent species coexisting, possibly in syntrophic interaction, may utilize motility to assist the spatial segregation often associated with phenotypic diﬀerentiation. Bioﬁlms represents till largely unexplored micro-cosmoses that will certainly provide numerous surprises in the future. In this Review, we have omitted the discussion of some crucial aspects in the life-cycle of a bioﬁlm: its ecology and genetic regulation. There is certainly ample space for physical theories of these diﬀerent levels of

a. action. b. Interaction c. accounts d. courses

Q105. arXiv: 1606.07419v1[cs.CV]23 June 2016: Learning to Poke by Poking: Experiential Learning of Intuitive Physics: Pulkit Agrawal, Ashvin Nair, Pieter Abbeel Jitendra Malik; {pulkitag, anair17, pabbeel, malik}@berkeley.edu; Sergey Levine; svlevine@cs.washington.edu; Abstract; We investigate an experiential learning paradigm for acquiring an internal model of intuitive physics. Our model is evaluated on a real-world robotic manipulation task that requires displacing objects to target locations by poking. The robot gathered over 400 hours of experience by executing more than 50K pokes on different objects. We propose a novel approach based on deep neural networks for modelling the dynamics of robot’s interactions directly from images, by jointly estimating forward and inverse models of dynamics. The inverse model objective provides supervision to construct informative visual features, which the forward model can then predict and in turn regularize the feature space for the inverse model. The interplay between these two objectives creates useful, accurate models that can then be used for multi-step decision making. This formulation has the additional beneﬁt that it is possible to learn forward models in an abstract feature space and thus alleviate the need of predicting pixels. Our experiments show that this joint modelling approach outperforms alternative methods. We also demonstrate that active data collection using the learned model further improves performance. We have proposed the use of intuitive models of physics learned from experience and simultaneous learning of forward and inverse models for vision based control. Although our approach is evaluated on a speciﬁc robotic manipulation task, there are no task speciﬁc assumptions, and the techniques are applicable to other tasks. In future, it would be interesting to see how the proposed approach scales with more complex environments, diverse object collections, and different manipulation skills and to other non-manipulation based tasks, such as

a. stream-lining b. imagination c. thoughts d. navigation

Q106. [physics. gen-ph] 19 June 2016: On some links between quantum physics and gravitation: Aleksey V. Ilyin; Moscow Institute of Physics and Technology (Dated: June 27, 2016) It is widely believed that quantum gravity eﬀects are negligible in a conventional laboratory experiment because quantum gravity should play its role only at a distance of about Planck’s length (∼10⁻³³ cm). Sometimes that is not the case as shown in this article. We discuss two new ideas about quantum physics connections with gravity. First, the Hong-Ou-Mandel eﬀect relation to quantum gravity is examined. Second, it is shown that the very existence of gravitons is an inevitable consequence of quantum statistics. Moreover, since the Bose-Einstein statistics is a special case of Compound Poisson Distribution, it predicts the existence of an inﬁnite family of high-spin massless particles that should be involved in gravitational interaction. In this work it is shown that the Hong-Ou-Mandel effect is directly related to quantum gravity. First, it is proven that coalescent photons appearing in the HOM eﬀect do not obey the Maxwell’s equations for electromagnetic ﬁeld. Second, strong arguments are given in favour of conclusion that two coalescent photons (referred to as a two-photon cluster) must obey the Einstein’s equations of general relativity. Therefore, a two-photon cluster is actually an optical frequency graviton. For this reason, the Hong-Ou-Mandel experiment [2] and many other HOM type experiments in the ﬁeld of quantum information are actually directly related to quantum gravity. In the second part of this work it is shown that quantum statistics probably high lights the direction of further development of gravitation theory. Indeed, today most physicists agree that the general theory of relativity in Einstein’s formulation is not the ultimate truth. This is true at least for two reasons: ﬁrstly, general relativity is incompatible with quantum physics; secondly, in general relativity inﬁnite solutions are unavoidable, which is unacceptable for a correct classical theory. However, it is well known, that Einstein’s equations are the only possible equations that may describe a spin-2 massless ﬁeld. Thus, further development of general relativity through modifying the equations for second rank tensor ﬁeld is impossible. The only real way of developing classical theory of gravitation is, therefore, to consider ﬁelds with higher spins. In this connection, Section III presents arguments showing that the existence of gravitons, as well as the existence of an inﬁnite family of massless ﬁelds of higher spins is an inevitable consequence of quantum statistics. The inﬁnite hierarchy of high-spin particles appears as a set of composite events in the Compound Poisson Distribution that describes the,

a. average statistics b. Fermi Statistics c. Grand Statistics d. Bose-Einstein Statistics

Q107. June 24, 2016: How van der Waals interactions determine the unique properties of water; Tobias Morawietz, Andreas Singraber, Christoph Dellago and J¨org Behler, Austria. While the interactions between water molecules are dominated by strongly directional hydrogen bonds (HBs), it was recently proposed that relatively weak, isotropic van der Waals (vdW) forces are essential for understanding the properties of liquid water and ice. This insight was derived from ab initio computer simulations, which provide an unbiased description of water at the atomic level and yield information on the underlying molecular forces. However, the high computational cost of such simulations prevents the systematic investigation of the inﬂuence of vdW forces on the thermodynamic anomalies of water. Here we develop eﬃcient ab initio-quality neural network potentials and use them to demonstrate that vdW interactions are crucial for the formation of water’s density maximum and its negative volume of melting. Both phenomena can be explained by the ﬂexibility of the HB network, which is the result of a delicate balance of weak vdW forces, causing e.g. a pronounced contraction of the second solvation shell upon cooling that induces the density,

a. minimum b. maximum c. threshold d. state

Q108. June 30, 2016; [astro-ph.HE]; SUPERNOVAE POWERED BY MAGNETARS THAT TRANSFORM INTO BLACK HOLES: TAKASHI J. MORIYA; takashi.moriya@nao.ac.jp; BRIAN D. METZGER 27, USA & SERGEI. I, Tokyo, ABSTRACT: Rapidly rotating, strongly magnetized neutron stars (magnetars) can release their enormous rotational energy via magnetic spin-down, providing a power source for bright transients such as superluminous supernovae. On the other hand, particularly massive (so-called supramassive) neutron stars require a minimum rotation rate to support their mass against gravitational collapse, below which the neutron star collapses to a black hole. We model the light curves of supernovae powered by magnetars which transform into black holes. Although the peak luminosities can reach high values in the range of superluminous supernovae, their post maximum light curves can decline very rapidly because of the sudden loss of the central energy input. Early black hole transformation also enhances the shock breakout signal from the magnetar-driven bubble relative to the main supernova peak. Our synthetic light curves of supernovae powered by magnetars transforming to black holes recently reported by Arcavi et al. (2016), are consistent with those of some rapidly evolving bright

a. transients b. bubbles c. collapses d. magnetars

Q.109. Dt.30 June 2016 [astro-ph.SR]: Fractal Reconnection in Solar and Stellar Environments: Kazunari Shibata and Shinsuke Takasao: Abstract: Recent space based observations of the Sun revealed that magnetic reconnection is ubiquitous in the solar atmosphere, ranging from small scale reconnection (observed as nanoﬂares) to large scale one (observed as long duration ﬂares or giant arcades). Often the magnetic reconnection events are associated with mass ejections or jets, which seem to be closely related to multiple plasmoid ejections from fractal current sheet. The bursty radio and hard X-ray emissions from ﬂares also suggest the fractal reconnection and associated particle acceleration. We shall discuss recent observations and theories related to the plasmoid-induced-reconnection and the fractal reconnection in solar ﬂares, and their implication to reconnection physics and particle acceleration. Recent ﬁndings of many superﬂares on solar type stars that has extended the applicability of the fractal reconnection model of solar ﬂares to much a wider parameter space suitable for stellar ﬂares are also discussed. If a super-ﬂare with energy 10³⁴ – 10 ³⁵ erg (i.e., 100 - 1000 times larger than the largest solar ﬂares ever observed, Carrington ﬂare) occurs on the present Sun, the damage that such a super-ﬂare can cause to our civilization would be extremely large; Hence it is very important to study the basic properties of super ﬂare on Sun-like stars to know the condition of occurrence of super-ﬂares and to understand how the super-ﬂares-producing stars are similar to our Sun. This is, of course, closely connected to the fundamental physics of reconnection: why and how fast reconnection occurs in magnetized plasma. Finally, we should note that stellar ﬂares sometimes show very bursty light curves in X-rays and visibile light, which is similar to bursty radio or HXR light curves of solar ﬂares during impulsive phase. This may be indirect evidence of turbulent (fractal) current sheet, since the fourier analysis of the time variability of the bursty light curve shows a power-law

a. average b. condition c. exponent d. distribution

Q110. [astro-phGA] 30 June 2016: .Dusty Quasars at High Redshifts: Daniel Weedman and Lusine Sargsyan: ABSTRACT: A population of quasars at z ∼ 2 is determined based on dust luminosities νLν(7.8 µm) that includes unobscured, partially obscured, and obscured quasars. Quasars are classiﬁed by the ratio νLν(0.25 µm)/νLν(7.8 µm) = UV/IR, assumed to measure obscuration of UV luminosity by the dust which produces IR luminosity. Quasar counts at rest frame 7.8 µm are determined for quasars in the Bo¨otes ﬁeld of the NOAO Deep Wide Field Survey using 24 µm sources with optical redshifts from the AGN and Galaxy Evolution Survey (AGES) or infrared redshifts from the Spitzer Infrared Spectrograph. Spectral energy distributions are extended to far infrared wavelengths using observations from the Herschel Space Observatory Spectral and Photometric Imaging Receiver (SPIRE), and new SPIRE photometry is presented for 77 high redshift quasars from the Sloan Digital Sky Survey. It is found that unobscured and obscured quasars have similar space densities at rest frame 7.8 µm, but the ratio Lν(100 µm)/Lν(7.8 µm) is about three times higher for obscured quasars compared to unobscured, so that far infrared or sub-mm discoveries are dominated by obscured quasars. Quasar source counts for these samples are determined for comparison to the number of sub-mm sources that have been discovered with the SCUBA-2 camera at z∼2 using the Lν(100 µm)/Lν(7.8 µm) results together with the Bo¨otes 7.8 µm counts, and we ﬁnd that only ∼ 5% of high redshift sub-mm sources are quasars, including even the most obscured quasars. Illustrative source counts are predicted to z = 10, and we show that existing SCUBA-2 850 µm surveys or 2 mm surveys with the Goddard-IRAM Superconducting 2 Millimeter Observer (GISMO) survey camera should already have detected sources at z∼10 if quasar and starburst luminosity functions remain the same from z = 2 until

a. z=100 b. z=3 c. z=10 d. z=11.

Q111. [ gr-qc] 29 June 2016; Axionic extension of the Einstein-aether theory: Alexander B. Balakin, n 420008, Russia (Dated: July 1, 2016): We extend the Einstein-aether theory to take into account the interaction between a pseudo-scalar ﬁeld, which describes the axionic dark matter, and a time-like dynamic unit vector ﬁeld, which characterizes the velocity of the aether motion. The Lagrangian of the Einstein-aether-axion theory includes cross-terms based on the axion ﬁeld and its gradient four-vector, on the covariant derivative of the aether velocity four-vector, and on the Riemann tensor and its convolutions. We follow the principles of the Eﬀective Field theory, and include into the Lagrangian of interactions all possible terms up to the second order in the covariant derivative. Interpretation of new couplings is given in terms of irreducible parts of the covariant derivative of the aether velocity, namely, the acceleration four-vector, the shear and vorticity tensors, and the expansion scalar. A spatially isotropic and homogeneous cosmological model with dynamic unit vector ﬁeld and axionic dark matter is considered as an application of the established theory; new exact solutions are discussed, which describe models with a Big Rip, Pseudo Rip and de Sitter-type asymptotic behaviour. Full-format phenomenological model of interactions between the gravitational ﬁeld, unit dynamic vector ﬁeld and pseudo-scalar (axion) ﬁeld is established as a model of the second order in the nomenclature of the Eﬀective Field theory. Master equations of this version of the Einstein-aether-axion theory are derived and presented. This phenomenological theory includes seventeen coupling parameters in addition to the standard constants c, G and Λ (see for the total action functional). In the spatially isotropic and homogeneous cosmological model only nine parameters (appearing with the expansion scalar Θ=3H(t)) from these seventeen constants are shown to be activated; other eight remain hidden parameters because of the symmetry of this model. The principle known as ”Occam’s razor” requires to reduce the wide set of phenomenological parameters to a minimal number of key coupling

a. variables b. constants c. parameters d. coefficients

Q112. [physics.atom-ph] 30 June 2016; Magnetic-ﬁeld-induced electric quadrupole moments for relativistic hydrogen-like atoms: Application of the Sturmian expansion of the generalized Dirac–Coulomb Green function: Patrycja Stefan´ska; Poland;Phys. Rev. A 93 (2016) 022504/1-11 :Abstract: We consider a Dirac one-electron atom placed in a weak, static, uniform magnetic ﬁeld. We show that, to the ﬁrst order in the strength B of the external ﬁeld, the only electric multipole moments, which are induced by the perturbation in the atom, are those of an even order. Using the Sturmian expansion of the generalized Dirac–Coulomb Green function [R. Szmytkowski, J. Phys. B 30, 825 (1997); 30, 2747(E) (1997)], we derive a closed-form expression for the electric quadrupole moment induced in the atom in an arbitrary discrete energy eigenstate. The result, which has the form of a double ﬁnite sum involving the generalized hypergeometric functions ₃F₂ of the unit argument, agrees with the earlier relativistic formula for that quantity, obtained by us for the ground state of the atom. We have analysed the electric multipole moments induced in the relativistic hydrogen-like atom in an arbitrary discrete energy eigenstate by a weak, uniform, static magnetic ﬁeld. We have shown that, to the ﬁrst order in the perturbing ﬁeld, only even-order electric multipole moments can be induced in the system. Next, we have derived analytically a closed-form expression for the induced electric quadrupole moment for any state of the Dirac one-electron atom. The result has the form of a double ﬁnite sum involving the generalized hypergeometric functions ₃F₂ of the unit argument; for the atomic ground state it reduces to the formula for the considered quantity found by us some time ago 2012. We have discussed this physical eﬀect on the basis of the relativistic theory and in a general overview. The result presented in this work not only has been obtained by taking into account the relativity, but also generalizes the existing formula for Q⁽¹⁾(B) to an arbitrary state of the atom. The calculations of the actual value of the induced electric quadrupole moment that we have carried out, provide another example of the usefulness of the Sturmian expansion of the generalized Dirac–Coulomb Green function for analytical determination of electromagnetic properties of the relativistic hydrogen-like atom in an arbitrary discrete energy

a. level b. state c. eigenstate d. eigenvalue.

Q113. [physics.general-ph]; 29 June 2016: Relations between the baryon quantum numbers of the Standard Model and of the rotating neutrino model: C.G. Vayenas, A.S. Fokas & D.P. Grigoriou; Greece, UK, USA; Abstract: We discuss the common features between the Standard Model taxonomy of particles, based on electric charge, strangeness and isospin, and the taxonomy emerging from the key structural elements of the rotating neutrino model, which describes baryons as bound states formed by three highly relativistic electrically polarized neutrinos forming a symmetric ring rotating around a central electrically charged or polarized lepton. It is shown that the two taxonomies are fully compatible with each other. The three quantum numbers of the SU(3) symmetry group of the Standard Model, namely charge, Q, Isospin, I₃, and strangeness, S, are analogous to the three quantum numbers, (Q, n_B and λ_B), which emerge from the rotating neutrino model. The baryon charge is determined by the charge, L, of the positron(s) or electron(s) located at the centre of the rotating neutrino ring. The maximum isospin value is also closely related to the number of leptons, L₊ and L₋, which can be accommodated at the centre of the rotating ring. Strangeness, on the other hand, is closely related both to the ﬁrst quantum number, n_B, and to the second quantum number, ℓ_B, which both dictate the value of the angular momentum and thus, via the Lorentz factor γ, the mass of the rotating neutrino baryon state given by m = n²_B(2ℓ_B + 1)]^1/6 3^13/12m^2/3 _Pl m^1/3 _o . This expression provides a very good ﬁt (R² > 0.996) to the masses of uncharmed baryons. Thus, in analogy with Bohr’s model of the H atom, it may turn out that the corresponding expressions for the Hamiltonians of these baryons, −(2/3) m_p [n²_B(2ℓ_B + 1)]^1/6 c² obtained via the rotating model, may be found in the future to be in reasonable agreement with the experimental values. However, the energies associated with transitions between such states are very high, in the far γ−ray range, and thus may be diﬃcult to

a. obtain b. guess c. revive d. contemplate.

Q114. Measuring neutrino mass imprinted on the anisotropic galaxy clustering; Minji Oh, Yong-Seon Song; Korea (Dated: July 6, 2016); The anisotropic galaxy clustering of large scale structure observed by the Baryon Oscillation Spectroscopic Survey Data Release 11 is analyzed to probe the sum of neutrino mass in the small mν<1eV limit in which the early broadband shape determined before the last scattering surface is immune from the variation of mν . The signature of mν is imprinted on the altered shape of the power spectrum at later epoch, which provides an opportunity to access the non--trivial mν through the measured anisotropic correlation function in redshift space (hereafter RSD instead of Redshift Space Distortion). The non--linear RSD corrections with massive neutrinos in the quasi linear regime are approximately estimated using one-loop order terms computed by tomographic linear solutions. We suggest a new approach to probe mν simultaneously with all other distance measures and coherent growth functions, exploiting this deformation of the early broadband shape of the spectrum at later epoch. If the origin of cosmic acceleration is unknown, mν is poorly determined after marginalising over all other observables. However, we find that the measured distances and coherent growth functions are minimally affected by the presence of mild neutrino mass. Although the standard model of cosmic acceleration is assumed to be the cosmological constant, the constraint on mν is little improved. Interestingly, the measured CMB distance to the last scattering surface sharply slices the degeneracy between the matter content and mν , and the hidden mν is excavated to be mν=0.19^+0.28_−0.17eV which is different from massless neutrino more than 68%

a. large b. more c. confidence d. limit

Q115. Mem. S. A. It. Vol. 75, 282, 2008; Compact Massive Objects in Galaxies; I. Tosta e Melo & R. Capuzzo-Dolcetta; iara.tosta.melo@gmail.com; Abstract. The central regions of galaxies show the presence of super massive black holes and/or very dense stellar clusters. Both objects seem to follow similar host-galaxy correlations, suggesting that they are members of the same family of Compact Massive Objects. We investigate here a huge data collection of Compact Massive Objects properties to correlate them with absolute magnitude, velocity dispersion and mass of their host galaxies. Our ﬁndings are: (i) galaxies brighter than M_B = −18 host SMBHs, and the existence of such objects in bright galaxies reconcile with the existence, in most of the cases, of an AGN. The lack of NSCs in faint galaxies may be related to the small number of globular clusters in galaxies; (ii) we reconﬁrmed that, with our updated set of data, as one moves to fainter galaxies, the nuclei become the dominant feature while MBHs tend to become less common and, perhaps, entirely disappear at the fainter end of the galaxy luminosity distribution; (iii) the M_NSC − σ correlation shows a slope between 1.5 and 3, which is in good agreement with theoretical ﬁndings by Arca-Sedda and Capuzzo-Dolcetta; (iv) as suggested by various theoretical-simulation scenarios, the dearth of NSCs in bright galaxies may be due to the presence of a single or binary SMBH which either evaporates the compact stellar structure or tidally destroy the in falling star

a. clusters b. groups c. events d. flares.

Q116. July 7, 2016 0:34: hep-ph: 5 July 2016: The Spin-Charge-Family theory oﬀers the explanation for all the assumptions of the Standard model, for the Dark matter, for the Matter-antimatter asymmetry, making several predictions: Norma Susana Mankoˇc Borˇstnik: Slovenia: The spin-charge-family theory, which is a kind of the Kaluza-Klein theories but with fermions carrying two kinds of spins (no charges), oﬀers the explanation for all the assumptions of the standard model, with the origin of families, the Higgs and the Yukawa couplings included. It oﬀers the explanation also for other phenomena, like the origin of the dark matter and of the matter/antimatter asymmetry in the universe. It predicts the existence of the fourth family to the observed three, as well as several scalar ﬁelds with the weak and the hyper charge of the standard model Higgs (±1/2,∓1/ 2, respectively), which determine the mass matrices of family members, oﬀering an explanation, why the fourth family with the masses above 1 TeV contributes weakly to the gluon-fusion production of the observed Higgs and to its decay into two photons and predicting that the two photons events, observed at the LHC at ≈ 750 GeV might be an indication for the existence of one of several scalars predicted by this theory. The possibility that the dark matter consists of clusters of the ﬁfth family - the stable heavy family of quarks and leptons (with zero Yukawa couplings to the lower group of four families) - is discussed. We made a rough estimation of the properties of baryons of this ﬁfth family members, of their behaviour during the evolution of the universe and when scattering on the ordinary matter. We studied possible limitations on the family properties due to the cosmological evidences, the direct experimental evidences, and all others (at that time) known properties of the

a. quark matter b. spin matter c. quark matter d. dark matter

Q117. [math.AP] 6 July 2016: AN INTRINSIC HYPERBOLOID APPROACH FOR EINSTEIN KLEIN-GORDON EQUATIONS: QIAN WANG: Abstract: Klainerman introduced the hyperboloidal method to prove the global existence results for nonlinear Klein-Gordon equations by using commuting vector ﬁelds. In this paper, we extend the hyperboloidal method from Minkowski space to Lorentzian space-times. This approach is developed for proving, under the maximal foliation gauge, the global nonlinear stability of Minkowski space for Einstein equations with massive scalar ﬁelds, which states that, the suﬃciently small data in a compact domain, surrounded by a Schwarzschild metric, leads to a unique, globally hyperbolic, smooth and geodesically complete solution to the Einstein Klein-Gordon system. In this paper, we set up the geometric framework of the intrinsic hyperboloid approach in the curved space-time. By performing a thorough geometric comparison between the radial normal vector ﬁeld induced by the intrinsic hyperboloids and the canonical ∂r, we manage to control the hyperboloids when they are close to their asymptote, which is a light cone in the Schwarzschild zone. By using such geometric information, we not only obtain the crucial boundary information for running the energy method, but also prove that the intrinsic geometric quantities including the Hawking mass all converge to their Schwarzschild values when approaching the

a. asymptote b. crosses c. invalids d. geometry.

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ANSWERS LIST

Q1.b. Q2.a. Q3.c. Q4.a. Q5.b. Q6.c. Q7.a. Q8.d. Q9.c. Q10.a. Q11.c. Q12.a. Q13.b. Q14.d. Q15.c. Q16.a. Q17.a. Q18.c. Q19.b. Q20.b. Q21.a. Q22.b. Q23.b. Q24.c. Q25.d. Q26.c. Q27.b Q28.d Q29.a. Q30.c. Q31.d. Q32.a. Q33.b. Q34.d. Q35.b. Q36.c. Q37.b. Q38.a. Q39.c Q40.a Q41.c. Q42.a. Q43.b. Q44.a. Q45.d. Q46.c. Q47.b. Q48.a. Q49.c. Q50.a. Q51.a. Q52.a. Q53.c. Q54.a. Q55.a. Q56.a. Q57.c. Q58.b. Q59.c. Q60.d. Q61.d. Q62.b. Q63.d. Q64.b. Q65.a. Q66.c. Q67.b. Q68.a. Q69.b. Q70.a. Q71.b. Q72.a. Q73.d. Q74.b. Q75.c. Q76.b. Q77.d. Q78.a. Q79.d. Q80.a. Q81.c. Q82.c. Q83.a. Q84.a. Q85.b. Q86.c. Q87.a. Q88.d. Q89.c. Q90.b. Q91.a. Q92.c. Q93.d. Q94.c. Q95.b. Q96.b. Q97.a. Q98.d. Q99.b. Q100.c. Q101.d. Q102.c. Q103.a. Q104.b. Q105.d. Q106.d. Q107.b. Q.108.a. Q109.d. Q110.c. Q111.b. Q112.c. Q113.a. Q114.c. Q115.a. Q116.d. Q117.a.

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TRU_SCIENCE & TRU_TECHNOLOGY

Thursday, September 8, 2016

TRUWIZ 117 in memory of Late Prof. K R Rao D.Sc.(Madras) D.Sc. (London)

a. Voids b. giants c. galaxies d. stars

a. Magnitude b. Value c. significance d. correction

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