September 09, 2022: TRUWIZ123b:

 September 09 2022: 

                                                      TRUWIZ 123b            

(see also truwiz123a)

trusciencetrutechnology@blogspot.com

Volume 2022, Dated: 09 September 2022

[Initiated by Prof. Dr. K. Lakshmi Narayana]

In Memory of

Late Professor Kotcherlakota Rangadhama Rao

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

(Birth on 09 September 1899 Early Morning, Berhampur, Demise on 20 June 1972 at 9 h 09 m at Visakhapatnam), at his residence, Narasimha Ashram, Official Colony, Maharanipeta. P. O., Visakhapatnam 530002. [Mrs. Peramma Rangadhama Rao demise on 31 Dec 1971 around 10 AM. at Narasimha Ashram, Official Colony, Maharanipeta.P.O.Visakhapatnam.]

                       TRUWIZ-123b.

Q63. arXiv:2201.04670 [astro-ph.SR]: Wed, 12 Jan 2022 19:48:48 UTC (80 KB)[Submitted on 12 Jan 2022]: Optical Photometry of WR140 as the Dust Formed During the 2016 Periastron Passage. Authors: Megan J. Peatt, Noel D. Richardson. :ABSTRACT: The colliding wind binary WR140 produces dust in its shocked gas every periastron passage. While the infrared light curve is very repeatable, there are noticeable changes every cycle in the optical time-series photometry. In the phases following periastron, there are optical dips in the light curve that were postulated to be caused by localized clumps in the dust produced in our line of sight. We report on the B and V-band light curves that were recorded by the American Association of Variable Star Observers (AAVSO) after the 2016 periastron event and briefly discuss comparisons to geometric models of the dust production to infer that these features are likely caused by localized dust clumps in the new dust 

                                                a. shell    b. cloud   c. phase   d. production.

Q64. arXiv:2201.05124 [astro-ph.GA]: Thu, 13 Jan 2022 18:28:26 UTC (1,591 KB)[Submitted on 13 Jan 2022]: Star formation near the Sun is driven by expansion of the Local Bubble. Catherine Zucker, et al., :ABSTRACT: For decades we have known that the Sun lies within the Local Bubble, a cavity of low-density, high-temperature plasma surrounded by a shell of cold, neutral gas and dust. However, the precise shape and extent of this shell, the impetus and timescale for its formation, and its relationship to nearby star formation have remained uncertain, largely due to low-resolution models of the local interstellar medium. Leveraging new spatial and dynamical constraints from the Gaia space mission, here we report an analysis of the 3D positions, shapes, and motions of dense gas and young stars within 200 pc of the Sun. We find that nearly all the star-forming complexes in the solar vicinity lie on the surface of the Local Bubble and that their young stars show outward expansion mainly perpendicular to the bubble's surface. Tracebacks of these young stars' motions support a scenario where the origin of the Local Bubble was a burst of stellar birth and then death (supernovae) taking place near the bubble's center beginning 14 Myr ago. The expansion of the Local Bubble created by the supernovae swept up the ambient interstellar medium into an extended shell that has now fragmented and collapsed into the most prominent nearby molecular clouds, in turn providing robust observational support for the theory of supernova-driven star 

                                       a. surface   b. bubble    c. formation.   d. swept.

Q65. arXiv:2201.07250 [astro-ph.GA]: Tue, 18 Jan 2022 19:00:02 UTC (32,066 KB)[Submitted on 18 Jan 2022]: Towards a More Complete Optical Census of Active Galactic Nuclei, Via Spatially-Resolved Spectroscopy. Julia M. Comerford, James Negus, R. Scott Barrows, Dominika Wylezalek, Jenny E. Greene, Francisco Müller-Sánchez, Rebecca Nevin. :ABSTRACT: While emission-line flux ratio diagnostics are the most common technique for identifying active galactic nuclei (AGNs) in optical spectra, applying this approach to single fiber spectra of galaxies can omit entire subpopulations of AGNs. Here, we use spatially resolved spectroscopy from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey to construct a sample of 10 galaxies where Baldwin-Philips-Terlevich line flux ratio diagnostics classify each galaxy's central 3′′ spectrum as LINER or star forming, while >10% of the spaxels in the galaxy's MaNGA footprint are classified as Seyfert. We obtain Chandra observations of these 10 galaxies with off-nuclear Seyfert regions to determine whether AGNs are actually present in them. Our main result is that 7-10 (depending on strictness of criteria) of the galaxies host one or more X-ray AGNs, even though none of them were classified as AGNs based on their single-fiber optical spectra. We find that these AGNs were not identified in the single-fiber spectra because they are AGNs in the nuclei of companion galaxies, low luminosity AGNs, dust obscured AGNs, and/or flickering AGNs. In summary, we find that off-nuclear AGN signatures may increase the number of known AGNs by a factor of two over what conventional single nuclear fiber spectra identify. Our results show that spatially resolved spectroscopy can be leveraged to reveal a more complete census of AGNs that are traditionally missed by single fiber 

                              a spectrum    b. spectra   c. luminosity  d. identity.

Q66.arXiv:2201.07271 [astro-ph.GA]: Tue, 18 Jan 2022 19:22:21 UTC (2,518 KB): [Submitted on 18 Jan 2022]: A fast radio burst progenitor born in a galaxy merger. :ABSTRACT: Balpreet Kaur, Nissim Kanekar, J. Xavier Prochaska. :ABSTRACT: We report a Giant Metrewave Radio Telescope HI 21cm mapping study of the neutral atomic hydrogen (HI) in the host galaxy of the fast radio burst (FRB) FRB20180916B at z≈0.03399. We find that the FRB host has an HI mass of MHI=(2.74±0.33)×10^9 M⊙ and a high HI-to-stellar mass ratio, ≈1.3. The FRB host is thus a gas-rich but near-quiescent galaxy, that is likely to have acquired a significant mass of HI in the recent past. The HI distribution is disturbed, with extended HI 21cm emission detected in a north-eastern tail, a counter-tail towards the south, an HI hole between the galaxy centre and the FRB location, and a high HI column density measured close to the FRB position. The FRB host is part of a group with four companions detected in their HI 21cm emission, the nearest of which is only 22~kpc from the FRB location. The gas-richness and disturbed HI distribution indicate that the FRB host has recently undergone a minor merger, which increased its HI mass, disturbed the HI in the galaxy disk, and compressed the HI near the FRB location to increase its surface density. We propose that this merger caused the burst of star-formation in the outskirts of the galaxy that gave rise to the FRB progenitor. The evidence for a minor merger is consistent with scenarios in which the FRB progenitor is a massive star, formed due to the merger 

                                    a.   event  b. formation   c. outskirt   d. group.

Q67. arXiv:2201.07507 [astro-ph.HE]: Wed, 19 Jan 2022 10:17:34 UTC (32 KB)[Submitted on 19 Jan 2022]: High magnetic field neutron stars and magnetars in binary systems. S.B. Popov. :ABSTRACT: Situation with highly magnetized neutron stars in binary systems is not yet certain. On the one hand, all best studied magnetars seem to be isolated objects. On the other, there are many claims based on model-dependent analysis of spin properties or/and luminosity of neutron stars in X-ray binaries in favour of large fields. In addition, there are a few results suggesting a magnetar-like activity of neutron stars in close binary systems. Most of theoretical considerations do not favour even existence, not speaking about active decay, of magnetar-scale fields in neutron stars older than ∼10^6 ~ yrs. However, alternative scenarios of the field evolution exist. I provide a brief review of theoretical and observational results related to the presence of neutron stars with large magnetic field in binaries and discuss perspectives of future 

                         a. thoughts   b. scenario   c. situations   d.studies.

Q68. arXiv:2201.07922 [astro-ph.CO:]Thu, 20 Jan 2022 00:04:47 UTC (89 KB)[Submitted on 20 Jan 2022]: Non-Gaussian Effects of the Saha's Ionization in the Early Universe. L. L. Sales, F. C. Carvalho, E. P. Bento, H. T. C. M. Souza:ABSTRACT: Tsallis' thermostatistical has received increasing attention due to its success in describing phenomena that manifest unusual thermodynamic properties. In this context, the generalized Saha equation must follow a condition of generalized thermal equilibrium of matter and radiation. The present work aims to explore the non-Gaussian effects on Saha's ionization via Tsallis statistics. To accomplish this, we generalized the number density taking into account a non-Gaussian Fermi-Dirac distribution, and then set out the Saha equation for the cosmological recombination. As a result, we highlight two new non-Gaussian effects: i) two generalized chemical equilibrium conditions, one for the relativistic regime and the other for the non-relativistic one; and ii) the hydrogen binding q-energy. We demonstrated that to yields smooth shifts in the binding energy, the a-parameter must be very small. We also showed that binding q-energy exhibits symmetrical behavior around the value of the standard binding energy. Besides, we used the q-energy in order to access other hydrogen energy levels, and we ascertained the values of the a-parameter that access those levels and their relationship to temperature. Finally, we employed these results to examine the non-Gaussian effects of the deuterium bottleneck, recombination and the particle anti-particle

                         a. extreme  b. excess  c. dominance   d. equation.

Q69. arXiv:2201.08345 [astro-ph.HE:]:Thu, 20 Jan 2022 18:26:40 UTC (6,799 KB)[Submitted on 20 Jan 2022]: Magnetic Field Evolution in Neutron Star Crusts: Beyond the Hall Effect. Konstantinos N. Gourgouliatos, Davide De Grandis, Andrei Igoshev:ABSTRACT: Neutron stars host the strongest magnetic fields that we know of in the Universe. Their magnetic fields are the main means of generating their radiation, either magnetospheric or through the crust. Moreover, the evolution of the magnetic field has been intimately related to explosive events of magnetars, which host strong magnetic fields, and their persistent thermal emission. The evolution of the magnetic field in the crusts of neutron stars has been described within the framework of the Hall effect and Ohmic dissipation. Yet, this description is limited by the fact that the Maxwell stresses exerted on the crusts of strongly magnetised neutron stars may lead to failure and temperature variations. In the former case, a failed crust does not completely fulfil the necessary conditions for the Hall effect. In the latter, the variations of temperature are strongly related to the magnetic field evolution. Finally, sharp gradients of the star's temperature may activate battery terms and alter the magnetic field structure, especially in weakly magnetised neutron stars. In this review, we discuss the recent progress made on these effects. We argue that these phenomena are likely to provide novel insight into our understanding of neutron stars and their observable 

                            a. dissipations. b. evolution   c. hall effect   d. properties.

Q70.arXiv:2201.08033 [physics.optics]: Thu, 20 Jan 2022 07:52:47 UTC (750 KB)[Submitted on 20 Jan 2022]: Porous SiO2 coated dielectric metasurface with consistent performance independent of environmental conditions. Authors: René Geromel,Christian Weinberger, Katja Brormann, Michael Tiemann, Thomas Zentgraf. :ABSTRACT: With the rapid advances of functional dielectric metasurfaces and their integration on on-chip nanophotonic devices, the necessity of metasurfaces working in different environments, especially in biological applications, arose. However, the metasurfaces' performance is tied to the unit cell's efficiency and ultimately the surrounding environment it was designed for, thus reducing its applicability if exposed to altering refractive index media. Here, we report a method to increase a metasurface's versatility by covering the high-index metasurface with a low index porous SiO2 film, protecting the metasurface from environmental changes while keeping the working efficiency unchanged. We show, that a covered metasurface retains its functionality even when exposed to fluidic 

                 a. systems   b. environments     c. metasurfaces   d. applicability.

Q71. JANUARY 26, 2022 / 04:48 PM IST: This startup is spinning yarn on solar charkhas, weaving fabric on solar looms and stitching clothes with solar sewing machines. Started in 2019 by NIFT Delhi graduate Abhishek Pathak, Greenwear has so far helped 3,500 women get trained in using solar spinning wheels. National Institute of Fashion Technology (NIFT) graduate Abhishek Pathak looks at the sun and weaves a dream for every day: Engage 5,000 women across India in spinning 5,000 metres of yarn on solar charkhas that would help weave 50,000 metres of fabric to be metamorphosed into 25,000 pieces of garment. All these on an every day basis. That looking at the sun is not an invocation of the gods, it is an integral part of Abhishek Pathak’s dream-weave - he is the founder and CEO of Greenwear, the country’s first brand for solar-vastra (yarn is spun on solar charkhas, fabric is woven on solar looms and garments are stitched on solar sewing machines). Incorporated in 2019, Greenwear offers a unique marketplace for eco-friendly, decentralised textile value chain, while generating livelihoods for rural women by addressing three key issues simultaneously - pollution by the fashion industry (fashion industry is the world’s second-largest polluter), poverty in rural India, and empowerment of rural women who comprise 81.29% of the total female workforce in India. It has been two years since Abhishek set out to become a solar vastra entrepreneur. So far, he has been instrumental is getting 3,500 women from UP, Bihar, Gujarat and Rajasthan trained in solar charkha skills, out of which 1,180 women got solar charkhas installed in their homes. In the coming years, Greenwear plans to enter new market segments like maternity wear, yoga wear, lounge wear, kids wear, hospital wear and hospitality wear. With two retail stores in Lucknow, Greenwear is also establishing its retail presence. “If only 5% of Indian villages become solar charkha clusters (around 30,000), it can produce 180 crore kilograms (18 lakh tonnes) of cotton yarn which is almost 50% of India’s current cotton yarn capacity and generate livelihood for 1.2 crore people without migrating from their villages,” Abhishek stared at the sun as he repeated his solar dream. A dream not only for himself but for those at the bottom of the economic 

              a. scenario  b. industry    c. workforce    d. pyramid.

Q72. arXiv:2201.11045 [astro-ph.GA]: Wed, 26 Jan 2022 16:41:11 UTC (10,931 KB)[Submitted on 26 Jan 2022]: The structure of accreted stellar streams. Yansong Qian, Yumna Arshad, Jo Bovy. :ABSTRACT: Many of the Milky Way's globular clusters are likely accreted from satellite galaxies that have long since merged with the Milky Way. When these globular clusters are susceptible to tidal disruption, this process likely starts already inside the parent satellite leading to an early stellar stream within the satellite. When the parent satellite merges with the Milky Way, the globular cluster and its pre-merger stellar stream are accreted in a somewhat chaotic process. Here, we investigate the properties of the accreted stream after the merger as we would see it today using a suite of simulations of accretion events. We find that the accretion process leads to a wide range of behaviors, but generally scatters the accreted stream over a wide, two-dimensional area of the sky. The behavior ranges from a set of a few or more well-defined "sub-streams" extending out from the post-merger thin stream by tens of degrees, to more widely dispersed debris over much of the sky, depending on how close to the center of the MilkyWay the merger happened. Using mock Gaia-like observations of the simulated streams, we demonstrate that an accreted-stream component can explain the off-track features observed in the GD-1 stream. Sub-streams can appear like thin tidal streams themselves that are seemingly unassociated with the post-merger stream, raising the possibility that some of the progenitor-less streams observed in the Milky Way are part of a single or a few accreted streams created in an ancient merger 

                                 a. dust   b. event    c. streams   d. process.

Q73. arXiv:2202.00684 [astro-ph.CO]:Tue, 1 Feb 2022 19:00:01 UTC (577 KB)[Submitted on 1 Feb 2022]: BICEP/Keck data and Quadratic Gravity.  Alberto Salvio. :ABSTRACT:  The recent results of the BICEP and Keck collaborations have put stringent bounds on many inflationary models, including some well-motivated ones. This is certainly the case when gravity remains described by Einstein's theory up to the inflationary scale, but can be avoided by introducing quadratic-in-curvature terms that are effective at that scale. Recently it has also been shown that these terms can UV complete gravity respecting stability and unitarity. Here the predictions of such quadratic gravity are computed and compared with the BICEP/Keck constraints by focusing on some of the inflationary scenarios that are best-motivated from the particle physics point of view and are already ruled out in Einstein gravity: (critical) Higgs inflation and natural inflation. The first scenario can be considered as the most economical option as the inflaton is identified with the only known elementary scalar field in the Standard Model and the near criticality of the Standard Model is used to remain in the perturbative regime. In the second one a pseudo-Nambu-Goldstone boson contributes to the inflationary dynamics and its potential is naturally flat. It is shown that in both scenarios one can restore the agreement with the observational constraints in quadratic 

                             a. gravity    b. form     c. inflation      d. scalr field.

Q74. arXiv:2202.00693 [astro-ph.GA]: Tue, 1 Feb 2022 19:00:03 UTC (2,005 KB)[Submitted on 1 Feb 2022]: Microwave Background Temperature at a Redshift of 6.34 from H2O Absorption. by Dominik A. Riechers, et al.,  : ABSTRACT: Distortions of the observed cosmic microwave background imprinted by the Sunyaev-Zel'dovich effect toward massive galaxy clusters due to inverse Compton scattering of microwave photons by high-energy electrons provide a direct measurement of the microwave background temperature at redshifts from 0 to 1. Some additional background temperature estimates exist at redshifts from 1.8 to 3.3 based on molecular and atomic line excitation temperatures in quasar absorption line systems, but are model dependent. To date, no deviations from the expected (1+z) scaling behavior of the microwave background temperature have been seen, but the measurements have not extended deeply into the matter-dominated era of the universe at redshifts z>3.3. Here we report the detection of sub-millimeter line absorption from the water molecule against the cosmic microwave background at z=6.34 in a massive starburst galaxy, corresponding to a lookback time of 12.8 Gyr. Radiative pumping of the upper level of the ground-state ortho-H2O(110-101) line due to starburst activity in the dusty galaxy HFLS3 results in a cooling to below the redshifted microwave background temperature, after the transition is initially excited by the microwave background. The strength of this effect implies a microwave background temperature of 16.4-30.2 K (1-sigma range) at z=6.34, which is consistent with a background temperature increase with redshift as expected from the standard CDM 

                             a. background   b. absorption  c. cosmology  d. starburst.

Q75.arXiv:2204.06003 [astro-ph.GA]:  Tue, 12 Apr 2022 18:00:00 UTC (31,352 KB); [Submitted on 12 Apr 2022]; The Radcliffe Wave as the gas spine of the Orion Arm. Cameren Swiggum, et al., :ABSTRACT: The Radcliffe Wave is a ∼3 kpc long coherent gas structure containing most of the star-forming complexes near the Sun. In this Letter we aim to find a Galactic context for the Radcliffe Wave by looking into a possible relationship between the gas structure and the Orion (Local) Arm. We use catalogs of massive stars and young open clusters based on \textit{Gaia} EDR3 astrometry, in conjunction with kiloparsec-scale 3D dust maps, to investigate the Galactic \textit{XY} spatial distributions of gas and young stars. We find a quasi-parallel offset between the luminous blue stars and the Radcliffe Wave, in that massive stars and clusters are found essentially inside and downstream from the Radcliffe Wave. We examine this offset in the context of color gradients observed in the spiral arms of external galaxies, where the interplay between density wave theory, spiral shocks, and triggered star formation has been used to interpret this particular arrangement of gas/dust and OB stars, and outline other potential explanations as well. We hypothesize that the Radcliffe Wave constitutes the gas reservoir of the Orion (Local) Arm, and presents itself as a prime laboratory to study the interface between Galactic structure, the formation of molecular clouds in the Milky Way, and star 

                            a. sustenance  b. formation     c. density   d. wave.

Q76.arXiv:2204.06010 [astro-ph.SR]:  Tue, 12 Apr 2022 18:00:04 UTC (7,184 KB)[Submitted on 12 Apr 2022]: Solar Flares and Magnetic Helicity. Authors: Shin Toriumi, Sung-Hong Park. ABSTRACT: Solar flares and coronal mass ejections are the largest energy release phenomena in the current solar system. They cause drastic enhancements of electromagnetic waves of various wavelengths and sometimes eject coronal material into the interplanetary space, disturbing the magnetic surroundings of orbiting planets including the Earth. It is generally accepted that solar flares are a phenomenon in which magnetic energy stored in the solar atmosphere above an active region is suddenly released through magnetic reconnection. Therefore, to elucidate the nature of solar flares, it is critical to estimate the complexity of the magnetic field and track its evolution. Magnetic helicity, a measure of the twist of coronal magnetic structures, is thus used to quantify and characterize the complexity of flare-productive active regions. This chapter provides an overview of solar flares and discusses how the different concepts of magnetic helicity are used to understand and predict solar 

                                       a. flares  b. disturbances   c. regions   d. material.       

Q77.arXiv:2204.06061 [astro-ph.SR]: Tue, 12 Apr 2022 19:47:40 UTC (35,576 KB)[Submitted on 12 Apr 2022]: Measuring Optical Extinction Towards Young Stellar Objects Using Diffuse Interstellar Bands. AUTHORS: Adolfo S. Carvalho, Lynne A. Hillenbrand. : ABSTRACT: Line-of-sight extinction estimates to well-studied young T Tauri and Herbig Ae/Be stars are based on many different measurements and analysis methods. This has resulted in wide scatter among the published AV values for the same star. In this work, we discuss the challenges in measuring extinction to actively accreting and especially outbursting young stellar objects (YSOs), and explore a method not previously applied to young stars, utilizing diffuse interstellar bands (DIBs). In early-type stars, narrow correlations exist between DIB equivalent widths and the column density of interstellar material, and therefore the line-of-sight extinction. Here, we measure equivalent widths of the 5780 Å and 6614 Å DIB features in a sample of actively accreting YSOs, and apply established DIB--reddening calibrations to derive reddening, and subsequently extinction. We also compare the DIBs-inferred optical line-of-sight extinction values with previous extinction estimates for our sample 

                                        a. galaxies    b. objects    c.  stars.    d. values.

Q78. arXiv:2204.06158 [astro-ph.HE]: Wed, 13 Apr 2022 03:49:07 UTC (1,154 KB): [Submitted on 13 Apr 2022]: Pulse Profiles and Polarization of Terzan 5 Pulsars. authors: Ashley R. Martsen,  et al., : ABSTRACT: Terzan 5 is a rich globular cluster within the galactic bulge that contains 39 known millisecond pulsars, the largest known population of any globular cluster. The Terzan 5 pulsars are faint, so that individual observations of most of the pulsars have too little signal-to-noise (S/N) to measure reliable flux density or polarization information. We combined over 5.2\,days of archival data, at each of 1.5\,GHz and 2.0\,GHz, taken with the Green Bank Telescope over the past 11\,years. We created high S/N profiles for 32 of the pulsars and determined precise rotation measures (RMs) for 28 of them. We used the RMs, and the known pulsar positions and dispersion measures (DMs), to map the projected parallel component of the Galactic magnetic field toward the cluster. The ⟨B||⟩ shows a rough gradient of ∼6\,nG/arcsec (∼160\,nG/parsec), or fractionally, a change of ∼20% in the right ascension direction across the cluster, implying Galactic magnetic field variability at sub-parsec scales. We also measured average flux densities Sν for the pulsars, ranging from ∼10\,μJy to ∼2\,mJy, and an average spectral index α=−1.35, where Sν∝να). This spectral index is flatter than most known pulsars, likely a selection effect due to the high frequencies used in pulsar searches to mitigate dispersion and scattering. The inferred pulsar luminosity function is roughly power-law, with slope (dlogN)/(dlogL)=−1 at the high-luminosity end. At the low-luminosity end, there are incompleteness effects implying that Terzan 5 contains many more pulsars to be 

                               a.  elaborated    b. found     c. detected     d. scattered.

Q79. May 07, 2021 at 6 PM: P rof. K. R. Rao D.Sc. (Madras). D.Sc. (London)  from 1919 to 1972 June 20, guided more than 70 doctoral Candidates at Andhra University, Waltair. He was in London and Sweden during the years 1928 to 1930, when he achieved D.Sc.(London). What is amazing is that he guided students from one end of spectrum, namely Radio Waves, through the intermediate ranges to Cosmic Rays, and many foreign scientists visited his laboratories in Andhra University, that claimed world wide recognition. Many of his students  migrated to USA and other countries. See his biography outlined by the present author Prof. Dr. Kotcherlakota Lakshmi Narayana in a series of articles. One British Lady took a lot of pains to collect all his original publications made in London etc., and made a volume of astounding memories of the extraordinary genius. Curtis was allowed but not Prof. K. R. Rao D.Sc.(London) permitted to board the ship to travel to USA in 1930. 

What I propose now that Prof. K. R. Rao thought of extended spectrum from far-below  the Radio Waves and as well far-beyond the Cosmic Rays. He cursorily mentioned it in his D. Sc. Thesis of Madras University, in the years 1919 to 1924, in-spite of most research work he carried  out in Vizianagaram and Visakhapatnam, with visits to Thiruvananthapuram. Amazingly he thought of the Quantum Spread of the Spectra and with limited resources he made very interesting statements of findings and about the observation of the Spectrums. 

Now I suggest that the electromagnetic Spectrum has a novel feature associated with the Quantum Spread, with the Spectrum extending below the Radio Waves and as well a far reaching extension above the Cosmic Rays,  

         a. unknown wave lengths. b. up the cosmic rays  c. spectrum   d. spread.

          [This write up was forwarded many who think interested in such writeups].

Q80. arXiv:2204.[physics.optics]:  Wed, 13 Apr 2022 08:15:55 UTC (1,708 KB): [Submitted on 13 Apr 2022]: Photonic quadrupole topological insulator using orbital-induced synthetic flux. AUTHORS. Julian Schulz, Jiho Noh, Wladimir A. Benalcazar, Gaurav Bahl, Georg von Freymann. : ABSTRACT: The rich physical properties of multiatomic molecules and crystalline structures are determined, to a significant extent, by the underlying geometry and connectivity of atomic orbitals. This orbital degree of freedom has also been used effectively to introduce structural diversity in a few synthetic materials including polariton lattices nonlinear photonic lattices and ultracold atoms in optical lattices. In particular, the mixing of orbitals with distinct parity representations, such as s and p orbitals, has been shown to be especially useful for generating systems that require alternating phase patterns, as with the sign of couplings within a lattice. Here we show that by further breaking the symmetries of such mixed-orbital lattices, it is possible to generate synthetic magnetic flux threading the lattice. This capability allows the generation of multipole higher-order topological phases in synthetic bosonic platforms, in which π flux threading each plaquette of the lattice is required, and which to date have only been implemented using tailored connectivity patterns. We use this insight to experimentally demonstrate a quadrupole photonic topological insulator in a two-dimensional lattice of waveguides that leverage modes with both s and p orbital-type representations. We confirm the nontrivial quadrupole topology of the system by observing the presence of protected zero-dimensional states, which are spatially confined to the corners, and by confirming that these states sit at the band gap. Our approach is also applicable to a broader range of time-reversal-invariant synthetic materials that do not allow for tailored connectivity, e.g. with nanoscale geometries, and in which synthetic fluxes are 

                          a.   importance    b. formidable    c. plaquettes.  d. essential.

Q81. arXiv:2204.06691 [astro-ph.EP]:  Thu, 14 Apr 2022 01:27:02 UTC (8,203 KB): [Submitted on 14 Apr 2022]: Gas and Dust Shadows in the TW Hydrae Disk. AUTHORS: Richard Teague, Jaehan Bae, Myriam Benisty, Sean M. Andrews, Stefano Facchini, Jane Huang, David Wilner. :ABSTRACT: We present new observations of CO J=2-1 emission from the protoplanetary disk around TW Hya. Emission is detected out to 240 au (4") and found to exhibit azimuthal variations up to 20% beyond 180 au (3"), with the west side of the disk brighter than the east. This asymmetry is interpreted as tracing the shadow previously seen in scattered light. A reanalysis of the multi-epoch observations of the dust shadow in scattered light from Debes et al. (2017) suggests that an oscillatory motion would provide a better model of the temporal evolution of the dust shadow rather than orbital motion. Both models predict an angular offset between the dust shadow and the gas shadow of up to ~100 deg. We attribute this offset to the finite rate at which dust grains and gas molecules can exchange heat, dominated by the collisional rate between gas molecules and dust grains, tcoll. The angular offsets derived are equivalent to collisional timescales that range from the near instantaneous up to tcoll ~ 10 years, depending on whether a straight or a curved dust shadow, as suggested by HST observations reported by Debes et al. (2017), is adopted. The inferred range of tcoll are consistent with those predictions based on representative gas densities, temperatures, gas-to-dust ratios and grain sizes. These results represent the first time empirical constraints can be placed on 

                            a.  tcoll  b. tcoll   c. temperatures   d. collisions.

Q82.arXiv:2204.07136 [astro-ph.HE]:  Thu, 14 Apr 2022 17:46:16 UTC (1,412 KB)[Submitted on 14 Apr 2022]: Constraining nucleosynthesis in neutrino-driven winds: observations, simulations and nuclear physics. AOUTHERS: A. Psaltis, A. Arcones, F. Montes, P. Mohr, C.J. Hansen, M. Jacobi, H. Schatz.  :ABSTRACT: A promising astrophysical site to produce the lighter heavy elements of the first r-process peak (Z=38−47) is the moderately neutron rich (0.4<Ye<0.5) neutrino-driven ejecta of explosive environments, such as core-collapse supernovae and neutron star mergers, where the weak r-process operates. This nucleosynthesis exhibits uncertainties from the absence of experimental data from (α,xn) reactions on neutron-rich nuclei, which are currently based on statistical model estimates. In this work, we report on a new study of the nuclear reaction impact using a Monte Carlo approach and improved (α,xn) rates based on the Atomki-V2 α Optical Model Potential (αOMP). We compare our results with observations from an up-to-date list of metal-poor stars with [Fe/H] < -1.5 to find conditions of the neutrino-driven wind where the lighter heavy elements can be synthesized. We identified a list of (α,xn) reaction rates that affect key elemental ratios in different astrophysical conditions. Our study aims on motivating more nuclear physics experiments on (α,xn) reactions using current and the new generation of radioactive beam facilities and also more observational studies of metal-poor 

                             a. colloids   b. stars   c. neutrinos    d. currents.

Q83. arXiv:2204.07068 [physics.ao-ph]:  Wed, 23 Mar 2022 12:42:25 UTC (1,789 KB)[Submitted on 23 Mar 2022]: Variation of Chaotic Behaviour of Wind Speed Oscillations Across Indian Subcontinent. :AUTHORS: G V Drisya, Alex Thumba. :ABSTRACT: Modelling the intermittency of wind speed has got significant relevance on many fields, including wind power generation and distribution. Most of the available modelling techniques assume the temporal fluctuations in the wind is stochastic in nature and the underlying dynamics is best described by statistical methods or the probabilistic distribution. The advent of chaos theory have changed the perception about irregular fluctuations of dynamic systems and it has demonstrated that random-like fluctuations can also arise from deterministic chaotic systems. In this paper, we have analysed the deterministic nature of apparent random fluctuations seen in the daily average wind speed with the help of nonlinear time series analysis tools utilising wind speed data measured at nine typical locations over the Indian subcontinent from 2005 to 2015. The values of significant chaotic quantifiers obtained from the analysis clearly show the deterministic, low-dimensional and chaotic nature of wind speed dynamics in all these

                              a. areas    b. regions   c. distributions   d. locations.

Q84. arXiv:2206.13528 [astro-ph.CO][Submitted on 27 Jun 2022]: Quasars as high-redshift standard candles. Authors: A. Sacchi, G. Risaliti, M. Signorini, E. Lusso, E. Nardini, G. Bargiacchi, S. Bisogni, F. Civano, M. Elvis, G. Fabbiano, R. Gilli, B. Trefoloni, C. Vignali. ABSTRACT: The non-linear relation between the X-ray and ultraviolet (UV) luminosity in quasars has been used to derive quasar distances and to build a Hubble diagram at redshifts up to z∼ 7. This cosmological application is based on the assumption of independence of the relation on redshift and luminosity. We want to test the reliability of this hypothesis by studying the spectroscopic properties of high-redshift quasars in the X-ray and UV bands. We performed a one-by-one analysis of a sample of 130 quasars at z> 2.5 with high-quality X-ray and UV spectroscopic observations. We found that not only the X-ray to UV correlation still holds at these redshifts, but its intrinsic dispersion is as low as 0.12 dex (previous works reached 0.20−0.22 dex). For a sample of quasars at z∼ 3 with particularly high-quality observations the dispersion further drops to 0.09 dex, a value entirely accountable for by intrinsic variability and source geometry effects. The composite spectra of these quasars, in both the X-rays and the UV, do not show any difference with respect to the average spectra of quasars at lower redshifts. The absence of any spectral difference between high- and low-z quasars and the tightness of the X-ray to UV relation suggests that no evolutionary effects are present in the relation. Therefore, it can be safely employed to derive quasar distances. Under this assumption, we obtain a measurement of the luminosity distance at z∼ 3 with 15 % uncertainty, and in a 4σ tension with the concordance 

                               a model b. example c. distance d. relation.

Q85. ArXiv: 2206.13535 [astro-ph.IM]: Mon, 27 Jun 2022 18:00:02 UTC (3,513 KB)[Submitted on 27 Jun 2022]: India's first robotic eye for time domain astrophysics: the GROWTH-India telescope. ABSTRACT: Harsh Kumar, et al., ABSTRACT: We present the design and performance of the GROWTH-India telescope, a 0.7 m robotic telescope dedicated to time-domain astronomy. The telescope is equipped with a 4k back-illuminated camera giving a 0.82-degree field of view and sensitivity of m_g ~20.5 in 5-min exposures. Custom software handles observatory operations: attaining high on-sky observing efficiencies (>~ 80%) and allowing rapid response to targets of opportunity. The data processing pipelines are capable of performing PSF photometry as well as image subtraction for transient searches. We also present an overview of the GROWTH-India telescope's contributions to the studies of Gamma-ray Bursts, the electromagnetic counterparts to gravitational wave sources, supernovae, novae and solar system objects.

                                   a. records b. fields c. objects d. views.

Q86. arXiv:2206.14834 [astro-ph.CO]: Wed, 29 Jun 2022 18:00:31 UTC (200 KB)[Submitted on 29 Jun 2022]: The Dynamical Mass of the Coma Cluster from Deep Learning. Authors: Matthew Ho, Michelle Ntampaka, Markus Michael Rau, Minghan Chen, Alexa Lansberry, Faith Ruehle, Hy Trac. ABSTRACT:  In 1933, Fritz Zwicky's famous investigations of the mass of the Coma cluster led him to infer the existence of dark matter \cite{1933AcHPh...6..110Z}. His fundamental discoveries have proven to be foundational to modern cosmology; as we now know such dark matter makes up 85\% of the matter and 25\% of the mass-energy content in the universe. Galaxy clusters like Coma are massive, complex systems of dark matter in addition to hot ionized gas and thousands of galaxies, and serve as excellent probes of the dark matter distribution. However, empirical studies show that the total mass of such systems remains elusive and difficult to precisely constrain. Here, we present new estimates for the dynamical mass of the Coma cluster based on Bayesian deep learning methodologies developed in recent years. Using our novel data-driven approach, we predict Coma's $\mthc$ mass to be $10^{15.10 \pm 0.15}\ \hmsun$ within a radius of 1.78±0.03 h^−1Mpc of its center. We show that our predictions are rigorous across multiple training datasets and statistically consistent with historical estimates of Coma's mass. This measurement reinforces our understanding of the dynamical state of the Coma cluster and advances rigorous analyses and verification methods for empirical applications of machine learning in 

                          a. Astrophysics.     b. astronomy       c. mass      d.   prediction.. 
Q87. arXiv:2206.14908 [astro-ph.GA]:  Wed, 29 Jun 2022 20:51:22 UTC (13,756 KB): [Submitted on 29 Jun 2022]: The Prime Focus Spectrograph Galaxy Evolution Survey. AUTHORS: Jenny Greene, Rachel Bezanson, Masami Ouchi, John Silverman, the PFS Galaxy Evolution Working Group. ABSTRACT: We present the Prime Focus Spectrograph (PFS) Galaxy Evolution pillar of the 360-night PFS Subaru Strategic Program. This 130-night program will capitalize on the wide wavelength coverage and massive multiplexing capabilities of PFS to study the evolution of typical galaxies from cosmic dawn to the present. From Lyman alpha emitters at z~7 to probe reionization, drop-outs at z~3 to map the inter-galactic medium in absorption, and a continuum-selected sample at z~1.5, we will chart the physics of galaxy evolution within the evolving cosmic web. This article is dedicated to the memory of Olivier Le Fevre, who was an early advocate for the construction of PFS, and a key early member of the Galaxy Evolution Working 

                         a. symmetry   b. facility      c. group      d.  galaxy

Q88.arXiv:2206.15151 [astro-ph.IM]:  Thu, 30 Jun 2022 09:35:03 UTC (8,726 KB)[Submitted on 30 Jun 2022]: A Route to Large-Scale Ultra-Low Noise Detector Arrays for Far-Infrared Space Applications. AUTHORS: D J Goldie, S. Withington, C. N. Thomas, P. A. R. Ade, R. V. Sudiwala. ABSTRACT: Far-infrared detectors for future cooled space telescopes require ultra-sensitive detectors with optical noise equivalent powers of order 0.2 aW/\sqrt Hz. This performance has already been demonstrated in arrays of transition edge sensors. A critical step is demonstrating a method of fabrication and assembly that maintains the performance but that is extendable to create large-scale arrays suitable, for example, for application in dispersive spectrometers where it may be advantageous to fabricate the array from smaller sub-arrays. Critical here are the methods of assembly and metrology that maintain the required tolerances on the spatial alignment of the components in order to maintain overall performance. These are discussed and 

                      a. demonstrated     b. illustrated      c. exemplified    d. detected.

Q89. arXiv:2207.00062 [astro-ph.GA]: Thu, 30 Jun 2022 18:52:36 UTC (2,434 KB) [Submitted on 30 Jun 2022]: Exploration of simple scenarios involving Fuzzy Dark Matter cores and gas at local scales. AUTHORS: I. Alvarez-Rios, F. S. Guzman. ABSTRACT: We introduce a tool that solves the Schrödinger-Euler-Poisson system of equations and allows the study of the interaction between ultralight bosonic dark matter, whose dynamics is described with the Schrödinger-Poisson system and luminous matter which, as a first approximation, is modeled with a single component compressible ideal fluid. The two matter fields are coupled through the Poisson equation, whose source is the addition of both, dark matter and gas densities. We describe the numerical methods used to solve the system of equations and present tests for each of the two components, that show the accuracy and convergence properties of the code. As simple possible applications we present some toy scenarios: i) the merger between a core of dark matter with a cloud of gas that could be the process of galaxy formation, ii) the merger of bosonic dark matter plus gas configurations emulating basic models of galaxy mergers, and iii) the post merger properties, including the dark-matter offset from gas and the correlation between oscillations of the bosonic core and those of the gas.

                    a.  source   b. components    c. gas      d. cloud.

Q90. arXiv:2207.00248 [astro-ph.HE]: Fri, 1 Jul 2022 07:40:05 UTC (1,370 KB):

[Submitted on 1 Jul 2022]: Pulse Frequency Fluctuations of Persistent Accretion

Powered.  Pulsars: AUTHORS: D. Serim, M. M. Serim, A. Baykal.  : ABSTRACT: In this

study, we  examine the long term torque noise fluctuations of persistent Xray binaries

Her X-1,  Vela X-1, GX 301-2, CEN X-3, 4U 1538-53, OAO 1657-415 and 4U 1626-67 using

the historical pulse frequency measurements provided by CGRO/BATSE and

Fermi/GBM. We find that known disk-fed sources exhibit 1/ω2 red noise component

in their power  density spectra which is saturated over long timescales. On the other

hand, wind-fed sources form a clear white noise component and the wind-fed sources

with occasional transient disk formation imprint 1/ω type flicker noise. We discuss their long-term

  timing noise properties based on the models to describe the power density spectrum

of pulse frequency derivative fluctuations in terms of monochromatic and colored 

noise processes. Furthermore, we investigate the relation between measured timing

  noise strengths and other independently measured physical parameters. Despite the 

low number of sample sources, we suggest that noise strengths of these sources are

correlated with their luminosities and uncorrelated with their magnetic fields strengths,

implying that the dominant noise generating mechanism is 

                       a. density   b. accretion    c. noise      d.  formation.

Q91. arXiv:2207.00337 [astro-ph.SR]: Fri, 1 Jul 2022 11:07:02 UTC (14,448 KB)

[Submitted on 1 Jul 2022]: Spectropolarimetry of Magnetic Chemically Peculiar Stars in the Orion OB1 Association. AUTHORS: Eugene Semenko, Iosif Romanyuk, Ilya Yakunin,

Dmitry Kudryavtsev, Anastasiya Moiseeva. :ABSTRACT: We summarise the results of a \spectropolarimetric survey of 56 chemically peculiar (CP) stars in the association of Orion

OB1. We uniformly collected the observational material with the 6-m telescope BTA of the

Special Astrophysical Observatory in 2013-2021. We identify 14 new magnetic CP stars

with a longitudinal magnetic field exceeding approximately 500 G. The studied sample

contains 31 magnetic stars or 55% of the whole CP population in Orion OB1. We show that

the percentage of the magnetic CP stars and the field strength drops sharply with age.

The mean longitudinal magnetic field in the young subgroup OB1b (logt=6.23) is confidently

almost three times stronger than in the older subgroups OB1a (logt=7.05) and

OB1c (logt=6.66). In the Orion Nebula, a place with the youngest stellar population (logt<6.0),

we detect the magnetic field only in 20% of CP stars. Such occurrence drastically differs

from 83% of magnetic CP stars in the nearby subgroup OB1c. We consider this effect an

observational bias caused by a significant portion of a very young population with the

signatures of Herbig Ae/Be stars. The technique we used for magnetic measurements,

and the quality of available data do not allow us to detect weak fields in the case of stars

with a limited number of lines and emissions in

a. population b. spectra c. drops d. CP .

Q93. arXiv:2207.00337 [astro-ph.SR]: Fri, 1 Jul 2022 11:07:02 UTC (14,448 KB):

[Submitted on 1 Jul 2022]: Title: Spectropolarimetry of Magnetic Chemically Peculiar

Stars in the Orion OB1 Association. AUTHORS : Eugene Semenko, Iosif Romanyuk,

Ilya Yakunin, Dmitry Kudryavtsev, Anastasiya Moiseeva. ABSTRACT: We summarise

the results of a spectropolarimetric survey of 56 chemically peculiar (CP) stars in

the association of Orion OB1. We uniformly collected the observational material

with the 6-m telescope BTA of the Special Astrophysical Observatory in 2013-2021.

We identify 14 new magnetic CP stars with a longitudinal magnetic field exceeding

approximately 500 G. The studied sample contains 31 magnetic stars or 55% of the

whole CP population in Orion OB1. We show that the percentage of the magnetic CP

stars and the field strength drops sharply with age. The mean longitudinal magnetic

field in the young subgroup OB1b (logt=6.23) is confidently almost three times stronger

than in the older subgroups OB1a (logt=7.05) and OB1c (logt=6.66). In the Orion Nebula,

a place with the youngest stellar population (logt<6.0), we detect the magnetic field

only in 20% of CP stars. Such occurrence drastically differs from 83% of magnetic CP

stars in the nearby subgroup OB1c. We consider this effect an observational bias

caused by a significant portion of a very young population with the signatures of

Herbig Ae/Be stars. The technique we used for magnetic measurements, and the quality

of available data do not allow us to detect weak fields in the case of stars with a limited

number of lines and emissions in

a. spectra b. CP c. OB1b d. 500G.

Q94.arXiv:2205.12282 [astro-ph.HE]: Thu, 7 Jul 2022 14:12:18 UTC (1,969 KB)

[Submitted on 24 May 2022 (v1), last revised 7 Jul 2022 (this version, v2)]:

Neutrino Emission from Luminous Fast Blue Optical Transients. : AUTHORS:

Ersilia Guarini, Irene Tamborra, Raffaella Margutti. ABSTRACT: Mounting evidence

suggests that Luminous Fast Blue Optical Transients (LFBOTs) are powered by a

compact object, launching an asymmetric and fast outflow responsible for the radiation

observed in the ultraviolet, optical, infrared, radio, and X-ray bands. Proposed

scenarios aiming to explain the electromagnetic emission include an inflated cocoon,

surrounding a jet choked in the extended stellar envelope. In alternative, the observed

radiation may arise from the disk formed by the delayed merger of a black hole with a

Wolf-Rayet star. We explore the neutrino production in these scenarios, i.e. internal

shocks in a choked jet and interaction between the outflow and the circumstellar

medium (CSM). If observed on-axis, the choked jet provides the dominant contribution

to the neutrino fluence. Intriguingly, the IceCube upper limit on the neutrino emission

inferred from the closest LFBOT, AT2018cow, excludes a region of the parameter space

otherwise allowed by electromagnetic observations. After correcting for the Eddington

bias on the observation of cosmic neutrinos, we conclude that the emission from an

on-axis choked jet and CSM interaction is compatible with the detection of two track-like

neutrino events observed by the IceCube Neutrino Observatory in coincidence with

AT2018cow, and otherwise considered to be of atmospheric origin. While the neutrino

emission from LFBOTs does not constitute the bulk of the diffuse background of

neutrinos observed by IceCube, detection prospects of nearby LFBOTs with IceCube

and the upcoming IceCube-Gen2 are encouraging. Follow-up neutrino searches will be

crucial for unravelling the mechanism powering this emergent transient a. division b. emissions c. class d. observation.

Q95. arXiv:2207.03541 [physics.optics]:  Thu, 7 Jul 2022 19:27:27 UTC (2,117 KB)[Submitted on 7 Jul 2022]: Title: Cherenkov radiation and scattering of external dispersive waves by two-color solitons. Authors: Ivan Oreshnikov, Oliver Melchert, Stephanie Willms, Surajit Bose, Ihar Babushkin, Ayhan Demircan, Uwe Morgner, Alexey Yulin. : ABSTRACT: For waveguides with two separate regions of anomalous dispersion, it is possible to create a quasi-stable two-color solitary wave. In this paper we consider how those waves interact with dispersive radiation, both generation of Cherenkov radiation and scattering of incident dispersive waves. We derive the analytic resonance conditions and verify them through numeric experiments. We also report incident radiation driving the internal oscillations of the soliton during the scattering process in case of an intense incident radiation. We generalize the resonance conditions for the case of an oscillating soliton and demonstrate how one can use the scattering process to probe and excite an internal mode of two-color soliton 

                            a. molecules   b. waves   c. dispersion     d. generation.

Q96. arXiv:2207.03649 [physics.optics]:   Fri, 8 Jul 2022 02:08:09 UTC (4,596 KB)[Submitted on 8 Jul 2022]: TITLE: High-speed laser writing of structural colors for full-color inkless printing. AUTHORS: Jiao Geng, Liye Xu, Wei Yan, Liping Shi, Min Qiu. :ABSTRACT: It is a formidable challenge to simultaneously achieve wide gamut, high resolution, high-speed while low-cost manufacturability, long-term stability, and viewing-angle independence in structural colors for practical applications. The conventional nanofabrication techniques fail to match the requirement in low-cost, large-scale and flexible manufacturing. Processing by ultrashort lasers can achieve extremely high throughput while suffering from a narrow gamut of 15% sRGB or angle-dependent colors. Here, we demonstrate an all-in-one solution for ultrafast laser-produced structural colors on ultrathin hybrid films that comprise an absorbent TiAlN layer coating on a metallic TiN layer. Under pulsed laser irradiation, the absorption behaviors of the TiAlN-TiN hybrid films are tailored by photothermal-induced oxidation on the topmost TiAlN. The oxidized films exhibit double-resonance absorption, which is attributed to the non-trivial phase shifts both at the oxide-TiAlN interface, and at the TiAlN-TiN interface. By varying the accumulated laser fluence to modulate the oxidation depth, an unprecedented large gamut of 90% sRGB is obtained. Our highly reproducible printing technique manifests angle-insensitive colors the variation of Hue is <0.14pi when viewing angles changing from 6 to 60. The full-color printing speed reaches to 1.4 cm2/s and the highest printing resolution exceeds 25000 dpi. The durability of the laser-printed colors is confirmed by fastness examination, including salt fog, double-85, light bleaching, and adhesion tests. These features render our technique to be competitive for high-throughput industrial 

                  a. methods    b. variations     c. accumulations      d.  applications.

Q97.arXiv:2207.03665 [cond-mat.soft]:  Fri, 8 Jul 2022 03:03:16 UTC (6,748 KB)[Submitted on 8 Jul 2022]: TITLE: Amorphous Entangled Active Matter. AUTHORS: William Savoie, Harry Tuazon, M. Saad Bhamla, Daniel I. Goldman. ABSTRACT: The design of amorphous entangled systems, specifically from soft and active materials, has the potential to open exciting new classes of active, shape-shifting, and task-capable 'smart' materials. However, the global emergent mechanics that arises from the local interactions of individual particles are not well understood. In this study, we examine the emergent properties of amorphous entangled systems in three different examples: an in-silico "smarticle" collection, its robophysical chain, and living entangled aggregate of worm blobs (L. variegatus). In simulations, we examine how material properties change for a collective composed of dynamic three-link robots. We compare three methods of controlling entanglement in a collective: externally oscillations, shape-changes, and internal oscillations. We find that large-amplitude changes of the particle's shape using the shape-change procedure produced the highest average number of entanglements, with respect to the aspect ratio (l/w), improving the tensile strength of the collective. We demonstrate application of these simulations in two experimental systems: robotic chains and entangled worm blobs. In the robophysical models, we find emergent auxeticity behavior upon straining the confined collective. And finally, we show how the individual worm activity in a blob can be controlled through the ambient dissolved oxygen in water, leading to complex emergent properties of the living entangled collective, such as solid-like entanglement and tumbling. Taken together, our work reveals principles by which future shape-modulating, potentially soft robotic systems may dynamically alter their material properties, advancing our understanding of living entangled materials, while inspiring new classes of synthetic emergent 

            a. solids     b. water     c. super materials      d. collections.

Q98. arXiv:2208.06492 [astro-ph.GA]:[Submitted on 12 Aug 2022]: Magnetic field properties in star formation: a review of their analysis methods and interpretation. by Junhao Liu (EAO), Qizhou Zhang (CfA), Keping Qiu (NJU): ABSTRACT: Linearly polarized emission from dust grains and molecular spectroscopy is an effective probe of the magnetic field topology in the interstellar medium and molecular clouds. The longstanding Davis-Chandrasekhar-Fermi (DCF) method and the recently developed Histogram of Relative Orientations (HRO) analysis and the polarization-intensity gradient (KTH) method are widely used to assess the dynamic role of magnetic fields in star formation based on the plane-of-sky component of field orientations inferred from the observations. We review the advances and limitations of these methods and summarize their applications to observations. Numerical tests of the DCF method, including its various variants, indicate that its largest uncertainty may come from the assumption of energy equipartition, which should be further calibrated with simulations and observations. We suggest that the ordered and turbulent magnetic fields of particular observations are local properties of the considered region. An analysis of the polarization observations using DCF estimations suggests that magnetically trans-to-super-critical and averagely trans-to-super-Alfvénic clumps/cores form in sub-critical clouds. High-mass star-forming regions may be more gravity-dominant than their low-mass counterparts due to higher column density. The observational HRO studies clearly reveal that the preferential relative orientation between the magnetic field and density structures changes from parallel to perpendicular with increasing column densities, which, in conjunction with simulations, suggests that star formation is ongoing in trans-to-sub-Alfvénic clouds. There is a possible transition back from perpendicular to random alignment at higher column densities. Results from observational studies using the KTH method broadly agree with those of the HRO and DCF 

                 a. reference   b. studies     c. abstracts     d. revelations.

Q99. arXiv:2208.06523 [astro-ph.EP]12 Aug 2022 22:58:04 UTC (2,455 KB):  [Submitted on 12 Aug 2022]: Thermal Evolution and magnetic history of rocky planets by Jisheng Zhang, Leslie Rogers.   : ABSTRACT: We present a thermal evolution model coupled with a Henyey solver to study the circumstances under which a rocky planet could potentially host a dynamo in its liquid iron core and/or magma ocean. We calculate the evolution of planet thermal profiles by solving the energy balance equations for both the mantle and the core. We use a modified mixing length theory to model the convective heat flow in both the magma ocean and solid mantle. In addition, by including the Henyey solver, we self-consistently account for adjustments in the interior structure and heating (cooling) due to planet contraction (expansion). We evaluate whether a dynamo can operate using the critical magnetic Reynolds number. We run simulations to explore how planet mass (Mpl), core mass fraction (CMF) and equilibrium temperature (Teq) affect the evolution and lifetime of possible dynamo sources. We find that the Teq determines the solidification regime of the magma ocean, and only layers with melt fraction greater than a critical value of 0.4 may contribute to the dynamo source region in the magma ocean. We find that the mantle mass, determined by Mpl and CMF, controls the thermal isolating effect on the iron core. In addition, we show that the liquid core last longer with increasing planet mass. For a core thermal conductivity of 40 Wm−1K−1, the lifetime of the dynamo in the iron core is limited by the lifetime of the liquid core for 1M⊕ planets, and by the lack of thermal convection for 3M⊕ 

                      a. planets   b. lifetimes    c. sources    d.  core.

Q100. arXiv:2208.06779 [astro-ph.SR]:  Sun, 14 Aug 2022 05:26:12 UTC (1,214 KB)[Submitted on 14 Aug 2022]: An outlook on the estimate of the solar quadrupole moment from relativistic gravitation contributions. AUTHORS: Jean-Pierre Rozelot, Ali Kilcik, Zahra Fazel: ABSTRACT: Of all the solar fundamental parameters (mass, diameter, gravity at the surface,...), the gravitational moments have been quite often ignored in the past, mainly due to the great difficulty to get a reliable estimate. Even though the order of magnitude of the solar quadrupole moment J2 is now known to be 10−7, its accurate value is still discussed. Indeed, the expansion in multipoles J(l, l=2,...) of the gravitational potential of a rotating body affects the orbital motion of planets at a relativistic level. We will recall here the recent progresses made in testing General Relativity through the contribution of the first solar quadrupole moment. Using the Eddington-Robertson parameters, we recall the constraints both on a theoretical and experimental point of view. Together with γ, which encodes the amount of curvature of space-time per unit rest-mass, the Post--Newtonian Parameter β c<ontributes to the relativistic precession of planets. The latter parameter encodes the amount of non-linearity in the superposition law of gravitation. Even though in principle, it would be possible to extract J2 from planetary ephemerides, we observe that it is significantly correlated with other solution parameters (semi-major axis of planets, mass of asteroids...). Focusing on the J2 correlations, we show that in general, when ~β and ~γ are freed, the correlations ~[β,J2] and ~[γ,J2] are ≈ 45\% and ≈ 55\% respectively. Moreover, all the planetary dynamics-based values are biased by the Lense--Thiring effect, which has never been modeled and solved for so far, but can be estimated to ≈ 7\%. It is thus possible to get a good estimate of the solar quadrupole moment:1.66×10−7≤J2≤

                         a. <= 2x10-7    b.  <= 5x10-7    c.  <= 4x10-7    d.  2.32x10-7

Q101.  arXiv:2208.07182 [astro-ph.HE]:  Mon, 15 Aug 2022 13:39:30 UTC (3,030 KB) [Submitted on 15 Aug 2022]: Spectral analysis of 22 radio pulsars using SKA-Low precursor stations. Authors: C. P. Lee, N. D. R. Bhat, M. Sokolowski, N. A. Swainston, D. Ung, A. Magro, R. Chiello. : ABSTRACT: We present the first observational study of pulsars performed with the second-generation precursor stations to the low-frequency component of the Square Kilometre Array (SKA-Low): the Aperture Array Verification System 2 (AAVS2) and the Engineering Development Array 2 (EDA2). Using the SKA-Low stations, we have observed 100 southern-sky pulsars between 70-350 MHz, including follow-up observations at multiple frequencies for a selected sample of bright pulsars. These observations have yielded detections of 22 pulsars, including the lowest-frequency detections ever published for 6 pulsars, despite the modest sensitivity of initial system where the recording bandwidth is limited to ~1 MHz. By comparing simultaneous flux density measurements obtained with the SKA-Low stations and performing rigorous electromagnetic simulations, we verify the accuracy of the SKA-Low sensitivity simulation code presented in Sokolowski et al. (2022). Furthermore, we perform model fits to the radio spectra of the detected pulsars using the method developed by Jankowski et al. (2018), including 9 pulsars which were not fitted in the original work. We robustly classify the spectra into 5 morphological classes and find that all but one pulsar exhibit deviations from simple power-law behaviour. These findings suggest that pulsars with well-determined spectra are more likely to show spectral flattening or turn-over than average. Our work demonstrates how SKA-Low stations can be meaningfully used for scientifically useful measurements and analysis of pulsar radio spectra, which are important inputs for informing pulsar surveys and science planned with the SKA-

                                    a.   High     b . Low      c. spectra       d. pulsars.

Q102. arXiv:2112.07645 [hep-th]:  Tue, 14 Dec 2021 18:46:55 UTC (73 KB),  Wed, 25 May 2022 05:15:55 UTC (75 KB),  Mon, 15 Aug 2022 09:07:25 UTC (76 KB):  [Submitted on 14 Dec 2021 (v1), last revised 15 Aug 2022 (this version, v3)]: Title: Axion anomalies. : Authors:  Peter Adshead, Kaloian D. Lozanov. :ABSTRACT:  We study fermions derivatively coupled to axion-like or pseudoscalar fields, and show that the axial vector current of the fermions is not conserved in the limit where the fermion is massless. This apparent violation of the classical chiral symmetry is due to the background axion field. We compute the contributions to this anomalous Ward identity due to the pseudoscalar field alone, which arise in Minkowski space, as well as the effects due to an interaction with an external gravitational field. For the case of massless fermions, these interactions induce terms in the axion effective action that can be removed by the addition of local counterterms. We demonstrate that these counterterms are generated by the transformation of the path integral measure when transforming the theory from a form where the chiral symmetry is manifest to one where the symmetry is only apparent after using the classical equations of motion. We work perturbatively in Minkowski space and include the effects of interactions with a linearized gravitational field. Using the heat kernel method, we study the transformation properties of the path integral measure, and include the effects of non-linear gravity as well as interactions with gauge fields. Finally, we verify our relation by considering derivatively coupled fermions during pseudoscalar-driven inflation and computing the divergence of the axial current in de Sitter spacetime.

                                        a.  world     b. theory   c. spacetime    d. time.

Q103. arXiv:2203.05396 [astro-ph.HE]:  Thu, 10 Mar 2022 14:41:51 UTC (869 KB)[Submitted on 10 Mar 2022 (v1), last revised 15 Aug 2022 (this version, v2)]: Externally-driven plasma models as candidates for pulsar radio emission. AUTHORS: Sk. Minhajur Rahaman, Dipanjan Mitra, George I. Melikidze.  ABSTRACT: Coherent radio emission from pulsars originates from excited plasma waves in an ultra-relativistic and strongly magnetized electron-positron pair plasma streaming along the open magnetic field lines of the pulsar. Traditional coherent radio emission models have relied on instabilities in this pair plasma. Recently alternative models have been suggested. These models appeal to direct coupling of the external electromagnetic field to the superluminal O-mode (lt2 mode) during the time-dependent pair cascade process at the polar gap. The objective of this work is to provide generic constraints on plasma models based on lt2 mode using realistic pulsar parameters. We find that the very short timescale associated with pair cascades does not allow lt2 mode to be excited at radio frequencies and the impulsive energy transfer can only increase the kinetic spread ("temperature") of the pair plasma particles. Moreover, under homogeneous plasma conditions, plasma waves on both branches of O-mode (i.e. superluminal lt2 and subluminal lt1) cannot escape the plasma. In the strongly magnetized pair plasma, only the extraordinary mode (t mode) can escape freely. We show that any generic fictitious mechanisms does not result in the wave electric field of t mode to have predominant orientation either parallel or perpendicular to the magnetic field plane as observed. Such fictitious mechanisms will inevitably lead to depolarization of signals and cannot account for the highly polarized single pulses observed in pulsars. We suggest coherent curvature radiation as a promising candidate for pulsar radio emission mechanism.

                            a. mechanism    b process   c. threshold     d. freely.

Q104. arXiv:2208.08208 [astro-ph.HE]: Wed, 17 Aug 2022 10:31:00 UTC (187 KB): [Submitted on 17 Aug 2022]: Title: The effects of plasma on the magnification and time delay of strongly lensed fast radio bursts. AUTHORS: Xinzhong Er, Shude Mao. :ABSTRACT: The number of identified Fast Radio Bursts (FRBs) is increasing rapidly with current and future facilities. Strongly lensed FRBs are expected to be found as well, which can provide precise time delays and thus have rich applications in cosmology and fundamental physics. However, the radio signal of lensed FRBs will be deflected by plasma in lens galaxies in addition to gravity. Such deflections by both gravity and plasma will cause frequency dependent time delays, which are different from the dispersion delay and the geometric delay caused by gravitational lensing. Depending on the lensing and plasma models, the frequency-time delay relation of the lensed images can show distinguishing behaviours either between the multiple images, or from the dispersion relation. Such phenomena cannot be neglected in future studies, especially at low radio frequency, as plasma exists in lens galaxies in general. More importantly, such information provides not only a potential way to search for lensed FRBs, but also constraints on the mass and plasma distributions in lens galaxy. In particular, plasma may make the missing central images observable at low radio 

                            a. time relation b. images  c. frequency   d. galaxy.

Q105. arXiv:2208.08050 [nucl-th]:Wed, 17 Aug 2022 03:42:59 UTC (4,789 KB): [Submitted on 17 Aug 2022]: TITLE: Neutrinos in Stellar Astrophysics: AUTHORS: G. M. Fuller, W. C. Haxton. :ABSTRACT: The physics of the mysterious and stealthy neutrino is at the heart of many phenomena in the cosmos. These particles interact with matter and with each other through the aptly named weak interaction. At typical astrophysical energies the weak interaction is some twenty orders of magnitude weaker than the electromagnetic interaction. However, in the early universe and in collapsing stars neutrinos can more than make up for their feeble interaction strength with huge numbers. Neutrinos can dominate the dynamics in these sites and set the conditions that govern the synthesis of the elements. Here we journey through the history of the discovery of these particles and describe their role in stellar evolution and collapse, the big bang, and multi-messenger astrophysics. Neutrino physics is at the frontier of elementary particle physics, nuclear physics, astrophysics and cosmology. All of these fields overlap in the neutrino 

                                        a. episode b. story  c. journey   d. evolution. 

Q107.arXiv:2208.08296 [hep-ph]: Wed, 17 Aug 2022 13:57:05 UTC (1,675 KB): [Submitted on 17 Aug 2022]: Title: Sneutrinos as two inflatons and curvaton and leptogenesis. :AUTHORS: Tomo Takahashi, Toshifumi Yamada, Shuichiro Yokoyama: ABSTRACT: We argue that sneutrinos can be embedded in a multi-field inflation framework where two inflatons and a curvaton simultaneously contribute to primordial fluctuations, which is consistent with current constraints on the spectral index and the tensor-to-scalar ratio from Planck and BICEP/Keck 2018. We also show that the same framework can also explain the baryon asymmetry of the Universe via leptogenesis realized by the decay of the lightest sneutrino. We investigate the parameter range for the scenario to work such as that of sneutrino masses. In particular, we show that the tensor-to-scalar ratio should be larger than 10−4 for a successful 

                     a. extract   b. sneutrinos   c. fluctuations    d. scenario.

Q108. arXiv:2208.07964 [cond-mat.mes-hall]: Tue, 16 Aug 2022 21:48:08 UTC (2,071 KB)[Submitted on 16 Aug 2022]: Mechanisms for Magnetic Skyrmion Catalysis and Topological Superconductivity. Authors: Yun-Peng Huang, Panagiotis Kotetes. :ABSTRACT: We propose an alternative route to stabilize magnetic skyrmion textures, which is free from the requirement of Dzyaloshinkii-Moriya interaction, magnetic anisotropy and the application of an external Zeeman field. Instead, it solely relies on time reversal symmetry (TRS) violation, and the emergence of flux in the ground state. We discuss scenarios that lead to a nonzero flux, and identify the possible magnetic ground states which become accessible in its presence. We focus on itinerant magnets with tetragonal symmetry, which preserve the full spin-rotational group but violate TRS. We demonstrate our mechanism for a concrete extended Dirac model, which can describe the protected surface states of a topological crystalline insulator. In addition, we investigate the topological phases obtained for the above extended Dirac model when two distinct magnetic skyrmion crystal ground states coexist with a conventional pairing gap. We find chiral topological superconducting phases, which harbor an integer number of chiral Majorana modes when line defects are present. Our mechanism opens alternative perspectives for engineering topological superconductivity in a minimal fashion. Evenmore, relaxing the stringent requirements to generate skyrmions, also promises to unlock new functional topological materials and devices which may be more compatible with electrostatic control than the currently explored skyrmion-Majorana 

                        a. platforms   b. fashion   c. mechanism    d. modes.

Q109. arXiv:2208.09042 [astro-ph.HE]: Thu, 18 Aug 2022 19:53:37 UTC (3,920 KB)[Submitted on 18 Aug 2022]:  The Early Evolution of Magnetar Rotation I: Slowly Rotating "Normal" Magnetars. Authors. Tejas Prasanna, Matthew S. B. Coleman, Matthias J. Raives, Todd A. Thompson. Abstract: In the seconds following their formation in core-collapse supernovae, "proto"-magnetars drive neutrino-heated magneto-centrifugal winds. Using a suite of two-dimensional axisymmetric MHD simulations, we show that relatively slowly rotating magnetars with initial spin periods of P⋆0=50−500 ms spin down rapidly during the neutrino Kelvin-Helmholtz cooling epoch. These initial spin periods are representative of those inferred for normal Galactic pulsars, and much slower than those invoked for gamma-ray bursts and super-luminous supernovae. Since the flow is non-relativistic at early times, and because the Alfvén radius is much larger than the proto-magnetar radius, spindown is millions of times more efficient than the typically-used dipole formula. Quasi-periodic plasmoid ejections from the closed zone enhance spindown. For polar magnetic field strengths B0≳5×10^14 G, the spindown timescale can be shorter than than the Kelvin-Helmholtz timescale. For B0≳10^15 G, it is of order seconds in early phases. We compute the spin evolution for cooling proto-magnetars as a function of B0, P⋆0, and mass (M). Proto-magnetars born with B0 greater than ≃1.3×10^15G(P⋆0/400ms)^−1.4 (M/1.4M⊙)^2.2 spin down to periods >1 s in just the first few seconds of evolution, well before the end of the cooling epoch and the onset of classic dipole spindown. Spindown is more efficient for lower M and for larger P⋆0. We discuss the implications for observed magnetars, including the discrepancy between their characteristic ages and supernova remnant ages. Finally, we speculate on the origin of 1E 161348-5055 in the remnant RCW 103, and the potential for other ultra-slowly rotating 

                              a.    stars    b. spindown   c. implications   d. magnetars.

Q110.  arXiv:2208.09196 [astro-ph.SR]:  Fri, 19 Aug 2022 07:41:53 UTC (656 KB)[Submitted on 19 Aug 2022]: Title: A decade-long magnetic monitoring of Vega. Authors: P. Petit, T. Böhm, C.P. Folsom, F. Lignières, T. Cang. : ABSTRACT: Aims. The very weak magnetic field detected at the surface of Vega hints at a widespread population of weakly magnetic stars of A and B spectral types. We contribute here to gather more clues about the origin of this magnetism by investigating the long-term stability of the field geometry of this prototypical star. Methods. We use spectropolarimetric data collected as part of a long-term campaign, with more than 2,000 observations spread between 2008 and 2018. Using various sub-sets extracted from the whole time series, we reconstruct several maps of the large-scale surface magnetic field. Results. We confirm that the polarimetric signal is modulated according to a ∼0.68 d period, which we interpret as the stellar rotation period. The surface magnetic field is organized in a complex geometry. We confirm the existence of a very localized, polar magnetic spot previously reported for Vega, with a radial field strength of about -5 G. We show that the surface of the star is also covered by a dipole, with a polar strength close to 9 G and a dipole obliquity close to 90∘. Both magnetic structures are remarkably stable over one decade. The available data suggest that smaller-scale magnetic spots may not be limited to the polar region, although the poor reliability of their reconstruction does not allow us to firmly conclude about their temporal 

                          a.     rotation      b . evolution      c.  geometry      d. strength.

Q111. arXiv:2208.09356 [astro-ph.SR]: Fri, 19 Aug 2022 14:10:09 UTC (296 KB): [Submitted on 19 Aug 2022]:Title: Infrared spectroscopy of the 2019 eruption of the recurrent nova V3890 Sgr: separation into equatorial and polar winds revealed. Authors: A. Evans (Keele University, UK), et al. ABSTRACT: We present infrared spectroscopy of the 2019 eruption of the recurrent nova V3890 Sgr, obtained over the period 5.1-46.3 days after the eruption. The spectrum of the red giant became more prominent as the flux declined, and by day 46.3 dominated the spectrum. Hydrogen and helium emission lines consisted of a narrow component superposed on a broad pedestal. The full width at half maximum of the narrow components declined with time t as the eruption progressed, as t^−0.74, whereas those of the broad components remained essentially constant. Conversely, the line fluxes of the narrow components of Pa,β remained roughly constant, while those of the broad components declined by a factor ∼30 over a period of ≲25~days. The behaviour of the broad components is consistent with them arising in unencumbered fast-flowing ejecta perpendicular to the binary plane, in material that was ejected in a short ∼3.3-day burst. The narrow components arise in material that encounters the accumulated circumstellar material. The outburst spectra were rich in coronal lines. There were two coronal line phases, one that originated in gas ionised by supersoft X-ray source, the other in shocked gas. From the relative fluxes of silicon and sulphur coronal lines on day 23.4 - when the emitting gas was shocked - we deduce that the temperature of the coronal gas was 9.3×10^5~K, and that the abundances are approximately 

                                        a. material   b. coronal     c. flux     d. solar.

Q112. arXiv:2208.09487 [astro-ph.SR]:  Fri, 19 Aug 2022 18:00:01 UTC (2,801 KB)[Submitted on 19 Aug 2022]: 30 to 100-kG magnetic fields in the cores of red giant stars. Authors: Gang Li, Sébastien Deheuvels, Jérôme Ballot, François Lignières. ABSTRACT: A red giant star is an evolved low- or intermediate-mass star that has exhausted its central hydrogen content, leaving a helium core and a hydrogen-burning shell. Oscillations of stars can be observed as periodic dimmings and brightenings in the optical light curves. In red giant stars, non-radial acoustic waves couple to gravity waves and give rise to mixed modes, which behave as pressure (p) modes in the envelope and gravity (g) modes in the core. These modes were previously used to measure the internal rotation of red giants, leading to the conclusion that purely hydrodynamical processes of angular momentum transport from the core are too inefficient. Magnetic fields could produce the additional required transport. However, due to the lack of direct measurements of magnetic fields in stellar interiors, very little is currently known about their properties. Asteroseismology can provide direct detection of magnetic fields because, like rotation, the fields induce shifts in the oscillation mode frequencies. Here we report the measurement of magnetic fields in the cores of three red giant stars observed with the Kepler satellite. The fields induce shifts that break the symmetry of dipole mode multiplets. We thus measure field strengths ranging from ~30 to ~100 kG in the vicinity of the hydrogen-burning shell and place constraints on the field 

                    a.   schemes   b. topology   c. properties   d.  measurements.

Q113. arXiv:2208.10164 [astro-ph.CO]:   Mon, 22 Aug 2022 09:21:43 UTC (3,850 KB): [Submitted on 22 Aug 2022]: Title: Minkowski Tensors in Redshift Space -- Beyond the Plane Parallel Approximation. AUTHORS: Stephen Appleby, Joby P. Kochappan, Pravabati Chingangbam, Changbom Park. :ABSTRACT: The Minkowski tensors (MTs) can be used to probe anisotropic signals in a field, and are well suited for measuring the redshift space distortion (RSD) signal in large scale structure catalogs. We consider how the linear RSD signal can be extracted from a field without resorting to the plane parallel approximation. A spherically redshift space distorted field is both anisotropic and inhomogeneous. We derive expressions for the two point correlation functions that elucidate the inhomogeneity, and then explain how the breakdown of homogeneity impacts the volume and ensemble averages of the tensor Minkowski functionals. We construct the ensemble average of these quantities in curvilinear coordinates and show that the ensemble and volume averages can be approximately equated, but this depends on our choice of definition of the volume average of a tensor and the radial distance between the observer and field. We then extract the tensor Minkowski functionals from spherically redshift space distorted, Gaussian random fields and gravitationally evolved dark matter density fields at z=0 to test if we can successfully measure the Kaiser RSD signal. For the dark matter field we find a significant, ∼10% anomalous signal in the MT component parallel to the line of sight that is present even on large scales RG≳15Mpc, in addition to the Kaiser effect. This is due to the line of sight component of the MT being significantly contaminated by the Finger of God effect, which can be approximately modelled by an additional damping term in the 

                            a   cumulants    b. fields    c. signals     d.  definition.

Q114. arXiv:2208.10363 [astro-ph.CO]:  Sun, 14 Aug 2022 08:03:36 UTC (16 KB)[Submitted on 14 Aug 2022]: Title: Looking for the Signals of the Missing Baryons in the Extragalactic Background Light. Authors: Wei Zhu, Rong Wang: ABSTRACT: The missing baryons in the universe are assumed to be hidden in the whole space as a warm-hot intergalactic medium (WHIM). Finding them is one of the important subjects in modern cosmology. In this paper, we point out that the very high energy electron/positron rays may light up the WHIM due to the anomalous bremsstrahlung according to the improved Bethe-Heitler formula. The resulting excess of the extragalactic background light (EBL) can be observed by the direct measurement method. A possible explanation on the difference between the direct and indirect measurements of EBL is also proposed. Thus, we open a new window to probe the WHIM properties via the 

                                              a.   EBB     b. RBC      c. EBL     d. EBF.

Q115. arXiv:2208.10532 [astro-ph.GA]:Mon, 22 Aug 2022 18:26:30 UTC (7,460 KB)[Submitted on 22 Aug 2022]: Title: CLASS: Coronal Line Activity Spectroscopic Survey. Authors: Michael Reefe, Shobita Satyapal, Remington O. Sexton, Sara M. Doan, Nathan J. Secrest, Jenna M. cann. :ABSTRACT: We conduct the first systematic survey of a comprehensive set of the twenty optical coronal lines in the spectra of nearly 1 million galaxies observed by the Sloan Digital Sky Survey (SDSS) Data Release 8 catalog. This includes often overlooked high ionization-potential (IP) lines such as [Ar X] λ5533, [S XII] λ7609, [Fe XI] λ7892, and [Fe XIV] λ5303. We find that, given the limited sensitivity of SDSS, strong coronal line emission is extremely rare, with only ∼0.03% of the sample showing at least one coronal line, significantly lower than the fraction of galaxies showing optical narrow line ratios (∼17%) or mid-infrared colors (∼2%) indicative of nuclear activity. The coronal line luminosities exhibit a large dynamic range, with values ranging from ∼1034 to 1042 erg s−1. We find that a vast majority (∼80%) of coronal line emitters in dwarf galaxies (M∗<9.6×109 M⊙) do not display optical narrow line ratios indicative of nuclear activity, in contrast to higher mass galaxies (∼17%). Moreover, we find that the highest ionization potential lines are preferentially found in lower mass galaxies. These findings are consistent with the theory that lower mass black holes found in lower mass galaxies produce a hotter accretion disk, which in turn enhances the higher ionization coronal line spectrum. Future coronal line searches with 30 m class telescopes or JWST may provide a pathway into uncovering the intermediate mass black hole 

                                    a. population     b. galaxies     c. emitters   d. displays.

Q116. arXiv:2208.10560 [astro-ph.CO]:  Mon, 22 Aug 2022 19:32:34 UTC (2,992 KB)[Submitted on 22 Aug 2022]: Title: Constraining effective neutrino species with bispectrum of large scale structures. Authors: Yanlong Shi, Chen Heinrich, Olivier Doré. : MABSTRACT: Relativistic and free-streaming particles like neutrinos leave imprints in large scale structures (LSS), providing probes of the effective number of neutrino species Neff. In this paper, we use the Fisher formalism to forecast Neff constraints from the bispectrum (B) of LSS for current and future galaxy redshift surveys, specifically using information from the baryon acoustic oscillations (BAOs). Modeling the galaxy bispectrum at the tree-level, we find that adding the bispectrum constraints to current CMB constraints from Planck can improve upon the Planck-only constraints on Neff by about 10\% -- 40\% depending on the survey. Compared to the Planck + power spectrum (P) constraints previously explored in the literature, using Planck+P+B provides a further improvement of about 5\% -- 30\%. Besides using BAO wiggles alone, we also explore using the total information which includes both the wiggles and the broadband information (which is subject to systematics challenges), generally yielding better results. Finally, we exploit the interference feature of the BAOs in the bispectrum to select a subset of triangles with the most information on Neff. This allows for the reduction of computational cost while keeping most of the information, as well as for circumventing some of the shortcomings of applying directly to the bispectrum the current wiggle extraction algorithm valid for the power spectrum. In sum, our study validates that the current Planck constraint on Neff can be significantly improved with the aid of galaxy surveys before the next-generation CMB experiments like CMB-

                                          a. stage 3   b .stage 2   c. stage 1    d. Stage 4.

Q117. arXiv:2208.10843 [astro-ph.SR]:  Tue, 23 Aug 2022 09:52:06 UTC (1,461 KB)[Submitted on 23 Aug 2022]: Title: The role of binarity and stellar rotation in the split main sequence of NGC 2422. Authors: Chenyu He, Weijia Sun, Chengyuan Li, Lu Li, Zhengyi Shao, Jing Zhong, Li Chen, Richard de Grijs, Baitian Tang, Songmei Qin, Zara Randriamanakoto.  :ABSTRACT: In addition to the extended main-sequence turnoffs widely found in young and intermediate-age (~ 600 Myr-2 Gyr-old) star clusters, some younger clusters even exhibit split main sequences (MSs). Different stellar rotation rates are proposed to account for the bifurcated MS pattern, with red and blue MSs (rMS and bMS) populated by fast and slowly rotating stars, respectively. Using photometry from Gaia Early Data Release 3, we report a Galactic open cluster with a bifurcated MS, NGC 2422 ( ~ 90 Myr). We exclude the possibilities that the bifurcated MS pattern is caused by photometric noise or differential reddening. We aim to examine if stellar rotation can account for the split MSs. We use spectra observed with the Canada-France-Hawaii Telescope and the Southern African Large Telescope, and directly measured v sin i, the projected rotational velocities, for stars populating the bMS and rMS. We find that their v sin i values are weakly correlated with their loci in the color-magnitude diagram because of contamination caused by a large fraction of rMS stars with low projected rotational velocities. Based on the spectral energy distribution fitting method, we suggest that these slowly rotating stars at the rMS may hide a binary companion, which breaks the expected v sin i-color correlation. Future time-domain studies focusing on whether these slowly rotating stars are radial velocity variables are crucial to test the roles of stellar rotation and binarity in generating the split 

                                          a. MS      b.  MSc      c. MSs    d.  MSS.

Q118. arXiv:2208.11026 [astro-ph.HE]:  Tue, 23 Aug 2022 15:12:18 UTC (10,356 KB)[Submitted on 23 Aug 2022]: TITLE: Pulsar Wind Nebulae. AUTHORS: A.M.W. Mitchell, J. Gelfand. :ABSTRACT: Pulsar Wind Nebulae (PWNe), structures powered by energetic pulsars, are known for their detection across the entire electromagnetic spectrum, with diverse morphologies and spectral behaviour between these bands. The temporal evolution of the morphology and spectrum of a PWN depends strongly on the properties of the associated neutron star, the relativistic outflow powered by its rotational energy, and surrounding medium, and thereby can vary markedly between objects. Due the continuous, but decreasing, injection of electrons and positrons into the PWN by the pulsar, the brightness and spectral variation within and amongst their wind nebulae reflect the magnetic field structure and particle transport within the PWN. This can include complex motions such as reverse flows or turbulence due to shock interactions and disruption to the nebula. During the last stage of the PWN's evolution, when the neutron star moves supersonically with respect to its environment, the escape of accelerated particles into the surrounding medium creates an extensive halo evident in very-high-energy gamma-rays. This chapter describes some of the identifying characteristics and key aspects of pulsar wind nebulae through their several evolutionary 

                                a. stages    b.  phases    c. environment     d.  evolution.

Q119. arXiv:2208.11689 [astro-ph.HE]: Wed, 24 Aug 2022 17:50:30 UTC (1,695 KB)[Submitted on 24 Aug 2022]:  Title: Limits on the nuclearite flux using the ANTARES neutrino telescope ANTARES Collaboration.  : ABSTRACT:In this work, a search for nuclearites of strange quark matter by using nine years of ANTARES data taken in the period 2009-2017 is presented. The passage through matter of these particles is simulated %according to the model of de Rújula and Glashow taking into account a detailed description of the detector response to nuclearites and of the data acquisition conditions. A down-going flux of cosmic nuclearites with Galactic velocities (β=10−3) was considered for this study. The mass threshold for detecting these particles at the detector level is \mbox{ 4×1013 GeV/c2}. Upper limits on the nuclearite flux for masses up to 1017 GeV/c2 at the level of ∼5×10−17 cm−2 s−1 sr−1 are obtained. These are the first upper limits on nuclearites established with a neutrino telescope and the most stringent ever set for Galactic velocities.

                          a. acceleration   b. particles   c. velocities    d. collaboration.

Q120. arXiv:2208.11234 [cond-mat.mes-hall]:  Tue, 23 Aug 2022 23:42:54 UTC (11,773 KB)[Submitted on 23 Aug 2022]: Title: Development of a Scanning Tunneling Microscope for Variable Temperature Electron Spin Resonance. AUTHORS: Jiyoon Hwang, Denis Krylov, Robertus J. G. Elbertse, Sangwon Yoon, Taehong Ahn, Jeongmin Oh, Lei Fang, Won-jun Jang, Franklin H. Cho, Andreas J. Heinrich, Yujeong Bae. :ABSTRACT: Recent advances in increasing the spectroscopic energy resolution in scanning tunneling microscopy (STM) have been achieved by integrating electron spin resonance (ESR) with STM. Here, we demonstrate the design and performance of a home-built STM capable of ESR at temperatures ranging from 1 K to 10 K. The STM is incorporated with a home-built Joule-Thomson refrigerator and a 2-axis vector magnet. Our STM design allows for the deposition of atoms and molecules directly into the cold STM, eliminating the need to extract the sample for deposition. In addition, we adopt two methods to apply radio-frequency (RF) voltages to the tunnel junction, the early design of wiring to the STM tip directly, and a more recent idea to use an RF antenna. Direct comparisons of ESR results measured using the two methods and simulations of electric field distribution around the tunnel junction show that, despite their different designs and capacitive couplings to the tunnel junction, there is no discernible difference in the driving and detection of ESR. Furthermore, at a magnetic field of 1.6 T, we observe ESR signals (near 40 GHz) sustained up to 10 K, which is the highest temperature for ESR-STM measurement reported to date, to the best of our knowledge. Although the ESR intensity exponentially decreases with increasing temperature, our ESR-STM system with low noise at the tunnel junction allows us to measure weak ESR signals with intensities in the sub-fA range. Our new design of ESR-STM, which is operational in a large frequency and temperature range, can broaden the use of ESR spectroscopy in STM and enable the simple modification of existing STM systems, which will hopefully accelerate a generalized use of ESR-

                                        a. STP       b. DRB      c. DEP     d. STM.

Q121.arXiv:2208.11421 [cond-mat.supr-con]:  Wed, 24 Aug 2022 10:40:20 UTC (1,363 KB)[Submitted on 24 Aug 2022]: Title: Plasmarons in high-temperature cuprate superconductors. Authors: Hiroyuki Yamase, Matias Bejas, Andres Greco. :ABSTRACT: Metallic systems exhibit plasmons as elementary excitations. This fundamental concept was reinforced also in high-temperature cuprate superconductors recently, although cuprates are not only layered systems but also strongly correlated electron systems. Here, we study how such ubiquitous plasmons leave their marks on the electron dispersion in cuprates. In contrast to phonons and magnetic fluctuations, plasmons do not yield a kink in the electron dispersion. Instead, we find that the optical plasmon accounts for an emergent band -- plasmarons -- in the one-particle excitation spectrum; acoustic-like plasmons typical to a layered system are far less effective. Because of strong electron correlations, the plasmarons are generated by bosonic fluctuations associated with the local constraint, not by the usual charge-density fluctuations, although both equally describe plasmons. Apart from this physical mechanism, a mathematical structure to host the plasmarons is similar to a weak coupling scheme discussed in alkali metals, Bi, graphene, monolayer transition-metal dichalcogenides, semiconductors, diamond, two-dimensional electron systems, and SrIrO3 films, establishing a concept of plasmarons in metallic systems in general. Plasmarons are realized below (above) the quasiparticle band in electron-doped (hole-doped) cuprates, including a region around (pi,0) and (0,pi) where the superconducting gap and the pseudogap are most 

                        a. superconducting    b. quasiparticle   c. enhanced   d.  systems.

Q122. arXiv:2208.09085 [nucl-th]:  Tue, 23 Aug 2022 01:43:20 UTC (602 KB): [Submitted on 18 Aug 2022 (v1), last revised 23 Aug 2022 (this version, v2)]: :Title: Early quark deconfinement in compact star astrophysics and heavy-ion collisions. :AUTHORS: Oleksii Ivanytskyi, David Blaschke, Tobias Fischer, Andreas Bauswein. :ABSTRACT: Based on a recently developed relativistic density functional approach to color-superconducting quark matter and a novel quark-hadron transition construction which phenomenologically accounts for the effects of inhomogeneous pasta phases and quark-hadron continuity, we construct a class of hybrid equations of state applicable at the regimes typical for compact star astrophysics and heavy ion collisions. We outline that early quark deconfinement is a notable consequence of strong diquark pairing providing a good agreement with the observational data and driving the trajectories of the matter evolution during the supernovae explosions toward the regimes typical for the compact star mergers and heavy-ion 

                                    a. collisions   b. trajectories   c. accounts   d.  data.

Q123. arXiv:2208.11708 [hep-ph]:  Wed, 24 Aug 2022 18:00:01 UTC (2,271 KB)[Submitted on 24 Aug 2022]: Title: Cascades of high-energy SM particles in the primordial thermal plasma. AUTHORS: Kyohei Mukaida, Masaki Yamada. :ABSTRACT: High-energy standard model (SM) particles in the early Universe are generated by the decay of heavy long-lived particles. The subsequent thermalization occurs through the splitting of high-energy primary particles into lower-energy daughters in primordial thermal plasma. The principal example of such processes is reheating after inflation caused by the decay of inflatons into SM particles. Understanding of the thermalization at reheating is extremely important as it reveals the origin of the hot Universe, and could open up new mechanisms for generating dark matter and/or baryon asymmetry. In this paper, we investigate the thermalization of high-energy SM particles in thermal plasma, taking into account the Landau--Pomeranchuk--Migdal effect in the leading-log approximation. The whole SM particle content and all the relevant SM interactions are included for the first time, i.e., the full gauge interactions of SU(3)C×SU(2)L×U(1)Y and the top Yukawa interaction. The distribution function of each SM species is computed both numerically and analytically. We have analytically obtained the distribution function of each SM species after the first few splitting's. Furthermore, we demonstrate that, after a sufficient number of splitting's, the particle distributions are asymptotic to certain values at low momentum, independent of the high-energy particles injected by inflation decay. The results are useful to calculate the DM abundance produced during the pre-thermal phase. An example is provided to illustrate a way to calculate the DM abundance from the scattering between the thermal plasma and high-energy particles in the 

                           a. splatting's    b.   first time    c. cascades    d. approximation.  

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TRUWIZ123b:  Dated:  9/9/2022 at  6:15 AM.

Q63a,Q64c,Q65b,Q66a,Q67d,Q68b,Q69d,Q70b,Q71d,Q72b,

Q73a,Q74c,Q75b,Q76a,Q77c,Q78b,Q79a,Q80d,Q81a,Q82b,Q83d,Q84a,Q85c,Q86b,Q87c,Q88a,Q89c,Q90b,Q91d,Q92b,

Q93a,Q94c,Q95a,Q96d,Q97c,Q98b,Q99a,Q100d,Q101b, 

Q102c,Q103a,Q104c,Q105b,Q106d,Q107b,Q108a,Q109d,

Q110b,Q111d,Q112b,Q113a,Q114c,Q115a,Q116d,Q117c, 

Q118a,Q119c,Q120d,Q121c,Q122a,Q123c.

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