TRUWIZ 116 Late Prof K R Rao D.Sc. (Madras) D.Sc. (London) B'Day Gift Presentation

TRUWIZ 116
trusciencetrutechnology@blogspot.com

Volume 2015, Issue No.9, Dated: 9 September 2015, 3.00 A.M

September 9, 2015

In Memory of

Late Professor Kotcherlakota Rangadhama Rao

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

(Birth on 9 September1899 Early Morning, Berhampur)

Demise on 20 June 1972 at 9h09m at Visakhapatnam,

at his residence, Narasimha Ashram

TRUWIZ-116

Q1. Ramayana is a real as several people in India firmly assert. Some say it dates back to one lakh fifty thousand years ago as late Rd. D. V. N. Sarma D.Sc. [unique five years] (AU) Ph. D. (USA) confirmed by the article he wrote on the bridge connecting India and Sri Lanka. The Deccan Chronicle on 18^th June 2015 quotes some Delhi University Professors assert that the communities Bhil, Kol and Gonda the major India Tribes acknowledged in epic Ramayana in Ayodhya Khanda, Aranya Khanda and Kishkindha Khanda. Gonds are found in Adilabad district and other states numbering about 40 lakh assert the Estonian Bio-centre in  DelhiIndian subcontinent can have ancestors dating back to what Late Dr. D. V. N.  Sarma of Chicago University, has found for eons ago!  Events described in Ramayana are

                   (a) Real (b) Optimistic (c) Unreal (d) Hypothetical.

Q2. Ground water from four longest basins depleting rapidly. Planet Earths’ largest aquifers between 2003 and 2013 were about 37.  No natural replenishment to offset usage in about

                   (a) Eight  (b) Ten  (c) Twelve (d) Twenty

Q3. An eye catching MX3D project to heat metal to 1500 deg. C before moulding it into place, printing with a six axis industrial robots, to build a functional life size steal bridge across a river in Netherlands. The arms would start at one end of the river and mechanically cross over to the other end using Robots to build a bridge. Work to begin in September 2015 at the city

                (a) Amsterdam (b) Uppsala (c) Cairo (d) London

Q4. Pepino, an exotic vegetable looks like a melon, it belongs to the   same family as tomato, potato, peppers and eggplant – Solanaceae. It is a shrub reaching to height of 150 cm, is profusely branched. The long-stalked fruits borne in clusters are of size 15-600gms. It is prized for its medicinal use. Storage is at

               (a) 5-10deg.C (b) 10-20deg.C (c) 20-30deg.C (d)30-40deg.C

Q5. High speed trains are three times energy efficient than cars and sixteen times more than

                (a) Motor cycles (b) steam ships (c) planes (d) satellites.

Q6. Placer or heavy (due to high specific gravity) minerals formed by mechanical concentration and natural gravity separation of mineral particles derived from weathered rocks, acidic or silicic rock-like granites and rhyolites have monazite, tourmaline and Zircon, while mafic rocks like gabbers and basalts contain ilmenite, magnetite, rutile etc., Metamorphic rocks as schist and gneiss host garnet, tourmaline, magnetite etc., hydrothermally formed rocks contain Cassiterite (tin), pyrite (iron sulphide), wolframite (tungsten), gold and

                  (a) Platinum (b) Silver (c) Copper (d) Gold

Q7. World’s fastest camera takes images at the rate of 4.4 trillion per second around one meter in length, capable of recording chemical reactions and heat conduction which occur at a sixth of the speed of light. The sequentially timed All-Optical Mapping photographs (STAMP) has resolution only 450x450 pixels. It uses femto-photography to capture images in a single burst.

                  (a) India (b) Japan (c) England (d) USA.

Q8. A scientist from India who is an Experimentalist cum Theoretician in Physics, play-math, biology, botany, archaeologist, as well of pioneer of Radio & Microwave, NQR, Optics research and an inventor of several research techniques is

                    (a) Prof. K. R. Rao (1899-1972) (b) Prof. Meghnad Saha

                    (c) Jagadish Chandra Bose (d) Homi J Bhabha.        

Q9. A research ship Sagar Manjusha, a multi-disciplinary research vessel designed by IMU, Visakhapatnam, with an overall length of 60m, gross  weight of 1075 MT at cruising speed of 6m/s at 90% MCR accommodates 8 officers and10 crew members has an endurance of about

                   (a) One month (b) 30 days (c) 60 days (d) one year.

Q10. Detailed studies of dynamics of galaxies and clusters of galaxies have indicated that there is appreciable amount of a

       (a) Dark Matter (b) Dark Energy (c) Luminous matter (d) galactic ether.   

Q11. The Greek borrowed from India all the ideas of Democracy, Philosophy, modern Medicine, Mathematics, Art and Science that can be traced back to the Muslim onslaught of India. Socrates knowledge, has two views in India as Jnana and Vijana. Plato concept of Love has both human and divine love in India. Aristotle thought of Science and Proof were borrowed from Ancient India. Ethics, logic and God discussions were predominant in India and left several treatises written by ancient experts and Scholars in India much before the Greek people thought about them. The female form, beauty and the male dominance were part of India culture as ancient sculptures and rock monuments aound and on the temples in India depict. Alexander left India with a great respect and full understanding. Words ‘Therefore’ and ‘Crisis’ were known to Indians and many a treatises both in Sanskrit and other Literature in have several elaborations and many of other multitudes of assertions in Indian grammer, Stoics and Mathematics. What made westerns think of the Genius exported from Greece?

            (a) Plato and Aristotle (b) Kreinein (decide) (c) Logic (d) Stoics  

Q12. A completely new view of the space-time structure its involvement with the Gravitons is envisaged and presented to account for terrestrial atmosphere presence of Pions, new Photons and new Anti-Photons. The diagrammatic approach to evaluate the matrix elements is given. The new current matrix elements of the graviton, with one - Pion state ⊞ (sum) new gamma, yields new mathematics of new Algebra, with novel sum ⊞.  The new photons have five projections to go with the similar Pions to match the Graviton of five projections +2, +1, 0, -1, -2. Similar expressions for the Anti-Graviton, Anti-Photon and the Anti-Pion are suggested and explicitly formulated by me. The effect of Gravity on virtual Pion-Gamma pairs as they propagate through space lead to a violation of Einstein’s equivalence principle while the effect is difficult to be measured being virtual its effects on creation of Muon-neutrino pairs and virtual Photons seems to be manageable. The analogous matrix element for the Anti-Photon is possible. (Paper presented at Ind. Sci. Cong. on 5^th January 2015 at Mumbai University, around 2h30mPM). The formulation hints at

               (a)  5D approach (b) Virtual Photons (c) Novel Sum (d) Anti-Photon.

Q13. INDORE: Threesome, all students of mechanical branch students of Indore Institute of Science and Technology (IIST), has developed a low-cost device that can print 3-dimensional (3D) objects. The indigenous printer creates 3D prototypes, which may be useful in industries such as architecture, construction, Industrial design, automotive, military, engineering and medical fields. The innovative machine has received a letter of appreciation from Raja Ramanna Centre for Advanced Technology, Indore (RRCAT) has offered students one-year internship under M Tech research programme of prestigious research and development institute. The device is a

                       (a)  Printer (b) program (c) exhibit (d) novelty.

Q14. WASHINGTON: New images of Ceres from Nasa's Dawn spacecraft has provided more visible images of mysterious bright spots and also revealed a pyramid-shaped peak towering over a relatively flat landscape. Dawn has been studying the dwarf planet Ceres, the largest object in the main asteroid belt between Mars and Jupiter, in detail from its second mapping orbit, which is 4,400 km above Ceres. A new view of its intriguing bright spots, located in a crater 90 km across, shows even more small spots in the crater than were previously visible, the US space agency said. At least eight spots can be seen next to the largest bright area, which scientists think is approximately wide

                        (a)  9km (b) 100km (c) 1000km (d) 2km

Q15. WASHINGTON: Researchers have created the world's thinnest light bulb using graphene, an atomically thin and perfectly crystalline form of carbon, as a filament.  Led by Young Duck Kim, a postdoctoral research scientist in James Hone's group at Columbia University School of Engineering, a team of scientists from Columbia, Seoul National University, and Korea Research Institute of Standards and Science said that they have demonstrated, for the first time, an on-chip visible light source using graphene as a filament.  They attached small strips of graphene to metal electrodes, suspended the strips above the substrate, and passed a current through the filaments to cause them to heat up. Hone Wang Fn-Jen Professor of mechanical engineering at Columbia Engineering said   "We've created what is essentially the world's thinnest bulb” of

                   (a) Sound (b) light (c) electricity (d) magnetism

 Q16. NEW YORK: Ever heard of a battery made of pulp? Here is one, developed by researchers from KTH Royal Institute of Technology, Sweden, and Stanford University, US, using nano-cellulose broken down from tree fibres, the researchers produced an elastic, foam-like battery material that can withstand shock and stress. "It is possible to make incredible materials from trees and cellulose," said researcher Max Hamedi from KTH.

                     (a) wood     (b) paper        (c) grass       (d) fruits

Q17.  MUMBAI: India is on the cusp of developing its own reusable space launch vehicle, popularly known as a space shuttle. Isro's 1.5 tonne vehicle resembling an aircraft is provisionally slated to make its maiden flight towards the end of July or August from the Satish Dhawan Space Centre, Sriharikota.   Officially known as the reusable launch vehicle (RLV-TD), it is undergoing final preparations at the Vikram Sarabhai Space Centre in Thiruvananthapuram. Its primary role will be to reduce the cost of access to space. The cost of placing 1kg of object in space is about $5,000, which scientists are hoping will come down with the RLV down to about

                           (a)  $900     (b) $600     (c)$700     (d) $500

Q18. WASHINGTON: The galaxy belongs to a new class of objects recently discovered by NASA's Wide-field Infrared Survey Explorer or WISE nicknamed extremely luminous infrared galaxies, or ELIRGs.   Scientists have discovered the most luminous galaxy in the universe to date that shines brightly with light equal to more than

                (a)  400 trillion Moons   (b) 300 trillion Suns

                (c) 500 trillion stars     (d) 600 trillion   galaxies

Q19.  On 23 June 2015 12:15 pm, Engineer Jill Hruby was named director of the Sandia National Laboratories on Monday, becoming the first woman to head one of three U.S. government labs charged with developing and maintaining the country’s nuclear arsenal. The 32-year veteran of the Albuquerque, New Mexico–based labs has overseen a wide range of research there, including studies focused on nuclear weapons, solar power, and machines that build miniscule electrical components the width of hair of

              (a) An animal (b) a monkey (c) a human (d) a chimpanzee

Q20. Prajnnaya Yagam before the Christ about 200 to 1000 years BC was performed in India. Sheshanalu earlier to Nannayya, (a first Telugu writer of Mahabarat translation from Sanskrit of 11^th century AC) depict these and perhaps are dependable. Hence Telugu songs existed even before 1^st century and Telugu literature was existing. Amaravathi sculpture word “Nagabu” earliest Telugu word! Satavahana, Ikshavakulu Sheshanams contains Telugu names of towns and people. Renati Cholas and eastern Chalukyas have Shashanalu made in Telugu. In 848 A.C. Panda Rangani Shashanamulu has “Patlambugattina Pradhamambu today BalaravamBhobaga Bailechisena Pattanbu Ghatiochi”  the “tharuvoja” poem one of the earliest poems on record. The sheshanam of 848 A.C. ”Poetic Prose” “Champu” style existed. Gunaga Vijayadhitya Kandhukuri sheshanam (848 A.C.) was an entirely poetic Telugu sheshanam. In 885 A.C. Yadhmaluni  Bezawada sheshanamu in Madhyakhor Chandasu (grammer) depicted in five poems. In 1000 A.C.  Viniyala kamasani (Gudur) sheshana has three Champakamala, and two Utpalamala poems. Poetic presentations and earlier to Nannaya “janapada”  literature existed ( Telugu literature History by Dr. D. N. Sastri October 1998. Telugu literature existed even before

             (a) 1^st century B.C.  (b)  1000 years B.C. (c) 200B.C (d)  400B.C.

Q21. Indian sculpture Science (Pancha Dasa kala) written by Swarna Subrahmanyam kavi Gandhinagar, Tenali 522201 September 2009 on page 85 at the end in the last sentence mentions two pigeons kept inside cages (panjaramulu) in the house of Mandana Misra Acharya discuss Vedanta discourses. “Pattinthicha” wood (Dharuvu) made Pigeons, Chilakulu, Pavuralu performing different dances with utterences of Vedic rythms stunned people. Mandana Misra became a disciple of

     (a) Ramanujacharaya (b) Sankaracharya  (c) Brughu maharshi (d) Vikramadhitya

Q22. Ujjaini city in 375-414 A.C. vikramadhitya ruled, who had 32 areas in his kingdom, and his thrown was surrounded by 32 images with mouths, that propagate distant sound either way presenting details of his lands and their welfare. To reply also there was machinery when meters pressed the news was being delivered by all the 32 channels. The machinery was termed as

           (a)   Yantramulu (b)  Sounders (c) Propagators (d) devices.

Q23.  In 230 B.C. to 225 B.C. Srimukha Satvahana Emperor (after Ikshavasksu) ruled in Dharanikonda (Dhanya Katakam) retold by Adavi Bapiraju in “Himabindu” novel (37-39 pages) possibly existing in

                 (a)  Madras (b) Kerala (c) Andhra (d) Karnataka.

Q24. Student excited for trip to study polar science.  July 13, 2015, 8:51 PM:  Aislinn Slaugenhaupt, from Pennsylvania, tells CBS News how excited she is about her trip to Greenland to study polar science, a student from 

               (a)   School   (b) Medium School (c) High school (d) lower school.

Q25. AsianScientist (Jul. 14, 2015):  Chemists at Pohang University of Science and Technology (POSTECH) have discovered an innovative method to form two-dimensional polyaniline (PANI) nano-sheets using ice as a hard template. Their results have been published in Angewandte Chemie and highlighted as a ‘Highly Important Paper’ by the journal. The product, called PANI-ICE, is reported to have distinctly outstanding electrical properties of low resistivity and high conductivity. PANI-ICE nano-sheets show high electronic current flows twice as high as that of graphene and over 40 times higher conductivity than PANI materials produced by existing established synthetic procedures. Among various conducting polymers, PANI has long been a promising candidate for practical applications, in particular for battery electrodes, due to its relatively simple chemical synthesis and easy doping process at a low financial and environmental cost, compared to

          (a)   Hard electronics (b) soft electronics (c) microelectronics (d) none.

Q26. The galaxy's microwave radiation can come from various processes including collisions between particles in the interstellar plasma (charged gas) and vibrations of dust grains caused by heat. But the particular wavelength of microwaves depicted in this map is created by something so unusual it's referred to as anomalous microwave emission, or AME for short. Scientists think AME may be caused by dust grains, the statement said by

               (a)  Collisions  (b) oscillations  (c) Spinning   (d) deposition

Q27. Faculty members also have opportunities to learn about industrial mathematics with their students. As a postdoc at Duke, I visited the United Kingdom and participated in a tradition called study groups (generally called math-in-industry workshops in the United States and Canada). In these intensive multi-day sessions, mathematicians and their students tackle problems presented by industry representatives. Students see their faculty mentors outside their usual professorial roles. If the solution presented by the team seems viable to the company, the group sometimes continues to work on the problem after the workshop. Thus, study groups can lead to continued associations between academic scholars and industry contacts, as well as internships or positions for faculty

                 (a)  Graduates (b) scholars (c) researchers  (d) academicians.

 28. Given n=10, σx=4.5, σy= 3.6, and sum of the product of deviation from the mean f x and y is 64.Find correlation coefficient r= Σ(xi - xˉ) (yi – y ˉ)  / (n  σx.σy )  yields r equal to

                        (a)  0.4    (b)  0.5    (c) 0.6    (d)  0.7

Q29. Solve x^2* y*dx  - (x^3 + y^3) *dy=0 to find

             (a) log y= x^3/(3y^3)  +  c       (b) log y=x^3 / (3 y^3)

             (b) log y= x^3                          (d) log y= 3y^3 

 

 

Q30. Solve d^3  y/ dx^3  -  8 y=0.

                     (a)  y=e^-x*c1 *cos √3 x           (b) e^-x * c2*sin √3 x

                     (c) y= e^-x * ( c1*cos√3 x + c2*sin √3x)           (d) none

Q31. Roberto de ‘Nobili went to India  in AD

                    (a) 1606 (b) 1608 (c) 1670 (d) 1700.

 Q32.When East India Company came to India? And established a factory?

(a)  1600 AD and Muslipatnam in 1639. (b) 1700 AD in Vizag and in 1730AD. (c) 1650 AD Bombay and Calcutta in 1670AD (d) 1620AD in Calcutta and Madras in 1650AD.

Q33. Who were the Muslims defeated in India to get control by British in Bengal, Carnatic coast, Mysore and Marathi regions.

(a)  Scraz D. Mir Jahani, Nawab of Bengal (b) Mir Kasim

             (c). Hyder Ali       (d) All in a, b, c and Tipu Sultan.

Q34. What is pale yellow brown shade like unbleached linen called?

                  (a) Ecru  (b)  Dcru (c) Fcru (d) Scru

Q35. Indian Queen who died in battle compared to queen Boadicia and Joan of Arc for her freedom

  (a).Rani Lakshmi Bai,  (b).Swaraj Lakshmi (c). Pingalli Venkata Ratnam (d). Jansi Rani 

   

Q36. Proverb of John Heywood (reprint from1598) when the Sun Shineth make

(a)  A day (b) Hay  (c) Meat (d) wine

Q37.  Weyl fermions detected in Tantalum Arsenide reports, Andrew Grant 2:00pm, July 16, 2015 EMail A kind of particle first predicted to exist before the discovery of Pluto has been spotted on Earth within a compound of tantalum and arsenic. The newly discovered particles, known as Weyl fermions, resemble massless electrons that dart around and through the material in unusual and exciting ways, researchers report July 16 in Science “It’s definitely a big deal,” says Leon Balents, a condensed matter theorist at the University of California, Santa Barbara. The particles’ behavior makes tantalum arsenide a metal-like compound that shares desirable features with graphene and topological insulators, materials that have attracted a torrent of research attention over the last

        (a)  Decade or so (b) ten years (c) thousand years (d) an year or so.

Q38. Some animals’ internal clocks follow a different drummer. Weird    an circadian rhythms keep organisms in time with their environments. Tina Hesman Saey, 1:00pm, July 14, 2015.  Migrating birds and newborn killer whales and bottlenose dolphins and their moms don’t sleep for weeks and may put their circadian clocks on snooze. Honeybees adjust their clocks according to their jobs in the hive. Nurses no longer follow the regular circadian cycles. Instead they care for larvae around the clock. A type of Mexican tetra (Astyanax mexicanus) that lives in dark caves has circadian clocks that are jammed in perpetual daytime. The unusual clock helps the fish save energy. Voles (Microtus arvalis) feed in 2- to 3-hour cycles of activity, known as “ultradian” rhythms. Ultradian means less than a day. Following circadian rhythms seems to be less important for the voles, raising the possibility that a shorter timer controls the ultradian activity cycles. In Arctic reindeer (Rangifer tarandus) the circadian clock has lost its rhythm or it beats only weakly. Going off the clock may help animals forage, sleep and carry out other activities in constant light and constant dark. The animals still follow seasonal cycles, such as mating and migration, dictated by a light-sensitive hormone called melatonin. Somalian cave fish, Phreatichthys andruzzii, haven’t seen the sun in more than a million years, but they still have the gears of standard circadian clocks. This clock no longer responds to light. It has wound down and now ticks out a 47-hour cycle, perhaps to synch with cyclical changes in the caves happening on that time scale. Or maybe the clock is slowly breaking because it no longer gives the fish an advantage. Some cicadas follow even longer clocks, emerging from underground every 13 to 17 years. No one knows how the insects mark time, says chrono biologist Barbara Helm of the University of Glasgow. The speckled sea louse Eurydice pulchra follows tidal rhythms so it knows when to burrow deep into the sand to avoid being swept out to sea and when to emerge to forage. The tidal clock is paced by a protein called casein kinase 1, which may be a gear left from an ancient clock upon which all others have been built. Along, with its circadian clock, a marine worm called Platynereis dumerilii has a timer set to the Moon, which controls when the animals spawn. No one has discovered yet which protein gears drive this lunar clock. But experiments have demonstrated that the lunar clockworks are different from those that keep the animal’s clock ticking of

                    (a)  Circadin  (b) heart beat  (c) speed  (d) looks

Q39. ‘’This is the first time we have had observational verification that large filamentary superhighways are channeling dwarf galaxies across the cosmos along magnificent bridges of dark matter.”  This cosmic “superhighway” gives the speeding satellites an off ramp along which they can be beamed toward the Milky Way, Andromeda, and Centaurus A. “The fact that this galactic bridge can affect the dwarf galaxies around us is impressive, given the difference in scale between the two, the planes of dwarfs are around 1 percent of the size of the galactic bridge to

          (a)  Virgo (b) Andromeda (c) Super-galaxy (d) Spica.

Q40. The two sets of stars are separated by about 21 billion km, rather larger than the size of Pluto's orbit around the Sun. The four stars were subsequently observed spectroscopically - its light was broken up into different wavelengths - so that the signatures of the different stars could be studied in detail. This unexpectedly revealed the presence of a fifth star, up to 2 billion km away from the detached binary, but not apparently producing any additional eclipses. By combining the data from the five stars' light curve and their spectra, the Open University researchers have been able to confirm that they are all gravitationally bound together in a single system, around 250 light years away from us in the constellation of Ursa Major. The data also let the team determine properties of the stars like their masses, sizes and temperatures. All the stars are rather smaller and cooler than our Sun, but the collective system is bright enough (9th magnitude) to be visible in small telescopes and amateur astronomers could see the eclipses for themselves. The light curve of the new quintuple system, designated as 1SWASP J093010.78+533859.5, initially revealed the presence of a contact eclipsing binary, a system in which the two stars are orbiting so close together that they share an outer atmosphere. Contact binaries are quite common, this particular system is notable because its orbital period, “the time the two stars take to complete one orbital cycle” is so but short, just under six hours. Then it was spotted that the light curve contained some additional unexpected eclipses, and the data were reanalysed to reveal a second eclipsing binary at the same location on the sky. The new binary is detached, its component stars are well-separated by a distance of about 3 million km, or about twice the size of the Sun and it has a longer orbital period of days

                      (a)  1-1/5    (b) 1-1/3    (c) 1-1/4   (d)1- 2/7

Q41. 07/16/15 10:09 AM EDT: Google announced Thursday it was strengthening its “Google Patents” search to help in determining whether a new patent application is valid. The search giant announced it will now allow people to search in one place for both previously patented material and other "prior art" that may be relevant to a patent application i.e.,

                      (a) New    (b) Old     (c) recent     (d) dedicated 

Q42. Sun-like stellar oscillations are excited by turbulent convection and have been discovered in some 500 main sequence and sub-giant stars and in more than 12,000 red giant stars. When such stars are near gravitational wave sources, low-order quadrupole acoustic modes are also excited above the experimental threshold of detectability, and they can be observed, in principle, in the acoustic spectra of these stars. Such stars form a set of natural detectors to search for gravitational waves over a large spectral frequency range, from 10⁻⁷ Hz to 10 ^-2   Hz. In particular, these stars can probe the 10⁻⁶ Hz – 10⁻⁴ Hz spectral window which cannot be probed by current conventional gravitational wave detectors, such as SKA and eLISA. The PLATO stellar seismic mission will achieve photospheric velocity amplitude accuracy of cm/s. For a gravitational wave search, we will need to achieve accuracies of the order of 10−2cm/s, i.e., at least one generation beyond PLATO. However, we have found that multi-body stellar systems have the ideal setup for this type of gravitational wave search. This is the case for triple stellar systems formed by a compact binary and an oscillating star. Continuous monitoring of the oscillation spectra of these stars to a distance of up to a kpc could lead to the discovery of gravitational waves originating in our galaxy or even elsewhere in the universe. Moreover, unlike experimental detectors, this observational network of stars will allow us to study the progression of gravitational waves throughout space.

                                      (a)  Galaxy  (b) time     (c) space      (d) universe

Q43. The layout of the quadrupolar field is such that positive fields emerge at the North and South poles, and negative fields are admitted at the limbs of the equator. This is similar to the order-2 convection harmonic on the Moon’s near side (see the web page He3 and Stellar Evolution for information on the Moon’s permanent, though remnant, quadrupole field). Before August 2012 scientists weren’t sure whether the quadrupole configuration would be permanent or temporary. The controversy started in the Autumn of 2011, when the Sun’s south polar region was observed to increase in field strength, not weaken as a precursor to flipping. In the Autumn of 2012 the magnetic field of the south pole finally showed signs of weakening. This began the normal trend towards a flip, and foiled any chance of a long-term asymmetry. Therefore the quadrupole configuration was temporary, The Sun is now (Feb. 2013) reverting to its normal dipole configuration and the quadrupole configuration was  

                  (a)  Random  (b) permanent  (c) oscillatory    (d) temporary

Q44. WASHINGTON (AP): In their annual, detailed physical of Earth's climate, scientists say the world is in increasingly hot and rising water. The National Oceanic and Atmospheric Administration and the American Meteorological Society's annual state of the climate report, released Thursday, delves into the details of already reported record-smashing warmth globally in 2014, giving special attention to the world's oceans. NOAA climate monitoring chief Deke Arndt, co-editor of the report, said the seas last year "were just ridiculous."  The report said ocean surface temperatures were the warmest in years of records, with the seas holding record levels of heat energy down to 2,300 feet below the surface. Sea level also hit modern highs, partly because warmer water expands.

                                 (a)  135   (b) 145   (c) 155  (d) 165

Q45. Parthenon of ancient Greece has golden ratio φ:1 (may be Human Head also has this ratio)  and Leonandoda Vinci in 16^th century published a book on golden ratio in

            (a) India (b) England (c) Italy (d) Hungary.

Q46. Technologies used for self-expression, human intercourse and recording of knowledge are in an un-precedent flux. A panoply of electronic devices puts everyone’s hand capacities far beyond anything that printing press could offer. Machines that think, allow people to do anything that could be done with communication tools of the past, and many more things too! The Yoga introduced at United Nations Assembly, by Narendra Modi engulfed the communication of several nations and is just only one

      (a) Communication tool (b) Exercise (c) Capacity (d) Human Culture.

Q47. Because density of Helium (mol.wt.4) is much less than that of air, a mixture of 78%Nitrogen (mol.wt.28) and 20% oxygen (mol. wt. 32) the vocal cards vibrate much faster (at a higher frequency )in Helium than in air, so the voice is perceived as having a pitch

                     (a)Lower (b) higher (c) intermediate (d) mixed

Q48. As haemoglobin loses its oxygen it turns a dark purplish blue, Deoxyhaemoglobin, which collects in larger veins, on its way back to the heart. Some fairly large veins lie just under the skin, where they appear blue, if there is not too much skin pigment (melanin) to hide the colour, the pigment is

                (a) Green (b) blue (c) brown (d) dark

Q49. Cambodia and Thailand calendars begin from death of Buddha. Hindu calendars begin from the birth of Brahma in the range of

                (a) Millennium (b) thousands (c) hundreds (d)  eons  

Q50. Why rain clouds are dark, when water particles become larger enough to form rain drops, they absorb light so they appear from below as

                     (a)White (b) Silvery (c) Dark (d) Grey. 

Q51. Why lightning has a zigzag pattern usually from cloud-to-ground and so through turbulent wind conditions that sends water droplets up the cloud while ice particles fall downward. The top of cloud carries the positive charge and bottom one carries a negative charge. Electrons shear off the rising droplets and stick to falling ice

             (a) Water drops (b) steam (c) crystals (d) lightning.

Q52. London (AFP) - Air pollution was the cause of the early deaths of almost 9,500 people in Britain's capital city in 2010, according to research by King's College London. The study showed for the first time the impact of nitrogen dioxide from exhaust fumes and fossil fuel burning, and showed the problem was far greater than previously thought. According to the study for Transport for London and the Greater London Authority, in 2010 there were 3,537 premature deaths in London due to particulate matter and due to nitrogen dioxide the deaths were

                      (a) 5879   (b) 6879   (c) 8879   (d)  9979

Q54. Heat was responsible for more deaths in the USA than any other weather-related cause between 2002 and 2011, says the National Weather Service. In that period, there were 1,185 heat deaths, compared with 1,139 hurricane deaths and 1,075 from tornadoes. People cool off Friday in Washington, D.C., where temperatures Lincoln, .also it was reported to Dr. Lalitha Kumari that the day temperatures were very high. They are

                      (a) 115   (b)   112    (c) 104   (d) 106

Q55.  Storms, lightning close LA beaches, causes power outages 39 minutes ago on 18^th July 2015, The Associated Press:   LOS ANGELES (AP), A rare summer storm has brought rain, thunder and lightning to Southern California, leading to beach closures and outages that left about 10,000 people without power. The threat of lightning strikes Qforced authorities to close 70 miles of Los Angeles County beaches as well as the popular Santa Monica Pier on Saturday afternoon. An Alaska Airlines jetliner was apparently struck after leaving Los Angeles International Airport, and was forced to return shortly after takeoff. An airport spokesman said the Washington D.C.-bound p lane landed safely.

                           (a) Thunder  (b) a jolt   (c) a flash of light  (d) Lightning

Q56. The  FIRSPEX  data  can  be  combined  with  a  multitude  of  existing  surveys, including line surveys, the 21cm line tracing HI in diffuse clouds, the 2.6mm CO J=1–0 transition tracing  molecular  clouds,  and  the  Hα  survey,  tracing  the  WIM, and  continuum  surveys, the  IR continuum tracing warm dust in regions of massive  star  formation as well with cold dust in atomic and molecular clouds, radio emissions at  several  wavelength  tracing  synchrotron emission due to relativistic  electrons  gyrating in the interstellar  magnetic  field, as well as free-free emission from gas ionized by massive stars, X-ray surveys of the tenuous hot gas (the Hot Inter-cloud Medium) generated by supernova explosions and filling the super-bubbles and chimneys in the ISM, and γ-ray surveys tracing the interaction of cosmic rays with atomic and molecular gas. The proposed FIRSPEX survey, together with this ancillary data, will address key questions on the origin and evolution of the interstellar medium such as: the energetics of the CNM and the WIM, the kinematics of the interstellar medium, the evolutionary relationship of atomic and molecular gas, the relationship of these ISM phases with newly formed stars, and the conversion of their radiative and kinetic power into thermal and turbulent energy of the ISM. The proposed survey will thus provide key insight in the lifecycle of the interstellar medium of the Milky Way.  Finally, it is worth stressing that one of the main technical drivers of ALMA is the ability to detect the C+ 158μm in normal galaxies in high redshift universe. Early results are already routinely used to determine the star formation rate in the early universe, despite that its origin in the Milky Way is not understood.  FIRSPEX will be key to turn these observations of the early universe into quantitative science with

(a)   Multitude of data (b) Red shifts (c) interstellar medium (d) Milky Way

Q57.. One view of the solar-wind turbulence is that the observed highly anisotropic fluctuations at spatial scales near the proton inertial length dp may be considered as Kinetic Alfv´en waves (KAWs).   In the present paper, we show how phase- mixing of large-scale parallel propagating Alfv´en waves is an efficient mechanism for the production of KAWs at wave-lengths  close to dp  and  at large propagation angle with  respect to the magnetic field. Magneto-hydrodynamic (MHD), Hall-Magneto-hydrodynamic (HMHD), and hybrid Vlasov-Maxwell (HVM) simulations modelling the propagation of Alfv´en waves in inhomogeneous plasmas are performed.  In linear regime, the role of dispersive effects is singled out by com-paring MHD and HMHD results.  Fluctuations produced by phase-mixing are identified as KAWs  through a comparison  of polarization of magnetic fluctuations and wave group velocity with analytical linear predictions. In the nonlinear regime, comparison of HMHD and HVM simulations allows to point out the role of kinetic effects in shaping the proton distribution function. We observe generation of temperature anisotropy with respect to the local magnetic field and production of field-aligned beams.   The regions where the proton distribution function highly departs from thermal equilibrium are located inside the shear layers, where the KAWs are excited, this suggesting that the distortions of the proton distribution are driven by a resonant interaction of protons with KAW fluctuations. Our results are relevant in configurations where magnetic field inhomogeneities are present, as, for example, in the solar corona where the presence of Alfv´en waves has been ascertained.

          (a) Solor Corona (b) KAWs  (c) Proton distribution (d) HMV

Q58. The new theory by Prof. Dr. K. L. Narayana, (23^rd July 2015) suggests that the DARK MATTER may be responsible for the traverse of the Mu particles long with their anti-Mu-neutrino, and a variety of Mu particles are released by their binding with the DARK MATTER. His new theory suggests possibly the number of DARK MATTER SCALARS as numbering about

                (a)  Four     (b)  three       (c)  Five      (d)  Six  

Q59. We investigate the Sun-Earth dynamics of a set of eight well observed solar coronal mass ejections (CMEs) using data from the STEREO spacecraft.   We seek to quantify the extent to which momentum coupling between these CMEs and the ambient solar wind (i.e., the aerodynamic drag) influences their dynamics. To this end, we use results from a 3D flux rope model fit to the CME data. We find that solar wind aerodynamic drag adequately accounts for the dynamics of the fastest CME in our sample.  For the relatively slower CMEs, we find that drag-based models initiated below heliocentric distances ranging from 15 to 50 R⊙ cannot account for the observed CME trajectories.  This is at variance with the general perception that the dynamics of slow CMEs are influenced primarily by solar wind drag from a few R⊙ onwards.  Several CMEs propagate at roughly constant speeds above 15–50 R⊙.  Drag-based models initiated above these heights therefore require negligible aerodynamic drag to explain their observed trajectories. CMEs move above 15-50 R⊙

                  (a)  Fast    (b) slowly    (c)Jumpy    (d) Hazard

Q60. Studying the neutrino in terrestrial experiments is a slow business. The neutrino is so ephemeral that experimenters must push the boundaries of technology and their patience in order to measure its physical properties.  But it is nature which pushes the envelope in the case of core-collapse supernovae  where one finds densities,  temperatures, magnetic fields etc. which far exceed anything we can  produce  here  on Earth. In such an environment neutrinos are no longer ghosts, they become important components of the system. A laundry list of properties of the neutrino alter the dynamics of the supernova and changes the signal we expect from the next supernova in our Galaxy.  This list includes both familiar standard model physics, such as the mass hierarchy, and BSM physics, such as non-standard interactions. Decoding the signal will be challenging but such sensitivity  to the neutrino means it would be wise for us to take  advantage  of this  immense potential  for probing  its  properties  (and to observe the inner  workings of the explosion) by preparing  for the day when the neutrinos eventually arrive, from the next  supernova

                    (a)  Ghosts  (b) Mass hierarchy   (c) Galactic  (d) Supernovae

Q61. We use data at 131, 171, and 304 ˚A from the Atmospheric Imaging Assembly (AIA) aboard  the Solar Dynamics  Observatory (SDO)  to search  for hot flux ropes in 141 M- class and  X-class solar flares that occurred  at solar longitudes equal to or larger  than 50◦ . Half of the flares were associated with coronal mass ejections (CMEs).  The goal of our survey is to assess the frequency of hot flux ropes in large flares irrespective of their formation time relative to the onset of eruptions.  The flux ropes were identified in 131˚A images using morphological criteria and their high temperatures were confirmed by their absence in the cooler 171 and 304 ˚A passbands. We found hot flux ropes in 45 of our events (32% of the flares); 11 of them were associated with confined flares while the remaining 34 were associated with eruptive flares.  Therefore almost half (49%) of the eruptive events involved a hot flux rope configuration.  The use of supplementary Hinode X-Ray Telescope (XRT) data indicates that these percentages should be considered as lower limits of the actual rates of occurrence of hot flux ropes in large flares, which are associated with

                   (a)  Solar Flares (b) X-ray flares   (c) CME   (d) Proton ejections.

Q62. We study water adsorption-induced deformation of a monolithic, mesoporous silicon (pSi) membrane traversed by independent channels of ~8 nm diameter. We focus on the elastic constant associated with the Laplace pressure-induced deformation of the membrane upon capillary condensation, i.e. the pore-load modulus. We perform finite-element method (FEM) simulations of the adsorption-induced deformation of hexagonal and square lattices of cylindrical pores representing the membrane. We find that the pore-load modulus weakly depends on the geometrical arrangement of pores, and can be expressed as a function of porosity. We propose an analytical model which relates the pore-load modulus to the porosity and to the elastic properties of bulk silicon (Young's modulus and Poisson's ratio), and provides an excellent agreement with FEM results. We find good agreement between our experimental data and the predictions of the analytical model, with the Young's modulus of the pore walls slightly lower than the bulk value. This model is applicable to a large class of materials with morphologies similar to mesoporous silicon. Moreover, our findings suggest that liquid condensation experiments allow one to elegantly access the elastic constants of a medium, which is

               (a) Porous (b) Mesoporous (c) Mega-porous (d) inhomogeneous

 Q63. We present a new analysis of the ratio €'/€ within the Standard Model (SM) using a formalism that is manifestly independent of the values of leading (V-A)®(V-A) QCD penguin, and EW penguin hadronic matrix elements of the operators Q₄, Q₉ and Q₁₀  and applies to the SM as well as extensions with the same operator structure. It is valid under the assumption that the SM exactly describes the data on CP-conserving K -> π π amplitudes. As a result of this and the high precision now available for CKM and quark mass parameters, to high accuracy epsilon'/epsilon depends only on two non-perturbative parameters, B₆^(1/2) and B₈^(3/2), and perturbative calculable Wilson coefficients. Within the SM, we are separately able to determine the hadronic matrix element ₄>_0 from CP-conserving data, significantly more precisely than presently possible with lattice QCD. Employing B₆^(1/2) = 0.57+-0.15 and B₈^(3/2) = 0.76+-0.05, extracted from recent results by the RBC-UKQCD collaboration, we obtain €'/€ = (2.23±.7) 10^-4, substantially more precise than the recent RBC-UKQCD prediction and more than 3σ below the experimental value (16.62±.3) 10^-4, with the error being fully dominated by that on B₆^(1/2). Even discarding lattice input completely, but employing the recently obtained bound B₆^(1/2) <= B₈^(3/2) <= 1 from the large-N approach, the SM value is found more than 2 sigma below the experimental value. At B₆^(1/2) = B₈^(3/2) = 1, varying all other parameters within one sigma, we find €'/€ = (9.13±.1) 10^-4. We present a detailed anatomy of the various SM uncertainties, including all sub-leading hadronic matrix elements, briefly commenting on the possibility of underestimated SM contributions as well as on the impact of our results on new Models

                 (a) Chemistry (b) Physics (c) Mathematical (d) Theoretical

Q64.  The field of particle physics is living very exciting times with a plethora of experiments looking for new physics in complementary ways. This has made increasingly necessary to obtain precise predictions in new physics models in order to be ready for a discovery that might be just around the corner. However, analyzing new models and studying their phenomenology can be really challenging. Computing mass matrices, interaction vertices and decay rates is already a tremendous task. In addition, obtaining predictions for the dark matter relic density and its detection prospects, computing flavor observables or estimating the LHC reach in certain collider signals constitutes quite a technical work due to the precision level that is currently required. For this reason, computer tools such as SARAH, MicrOmegas, MadGraph, SPheno or FlavorKit have become quite popular, and many physicists use them on a daily basis. In this course we will learn how to use these computer tools to explore new physics models and get robust numerical predictions to probe them in current and future experiments.

                    (a)  Practical   (b) Assertive   (c) numerical   (d) predictive

Q65. The Planck mission, thanks to its large frequency range and all-sky coverage, has a unique potential for systematically detecting the brightest, and rarest, sub-millimeter sources on the sky, including distant objects in the high-redshift Universe traced by their dust emission. A novel method, based on a component-separation procedure using a combination of Planck and IRAS data, has been applied to select the most luminous cold sub-mm sources with spectral energy distributions peaking between 353 and 857GHz at 5' resolution. A total of 2151 Planck high-z source candidates (the PHZ) have been detected in the cleanest 26% of the sky, with flux density at 545GHz above 500mJy. Embedded in the cosmic infrared background close to the confusion limit, these high-z candidates exhibit colder colors than their surroundings, consistent with redshifts z>2, assuming a dust temperature of 35K and a spectral index of 1.5. First follow-up observations obtained from optical to sub-mm have confirmed that this list consists of two distinct populations. A small fraction (around 3%) of the sources have been identified as strongly gravitationally lensed star-forming galaxies, which are amongst the brightest sub-mm lensed objects (with flux density at 545GHz ranging from 350mJy up to 1Jy) at redshift 2 to 4. However, the vast majority of the PHZ sources appear as over densities of dusty star-forming galaxies, having colors consistent with z>2, and may be considered as proto-cluster candidates. The PHZ provides an original sample, complementary to the Planck Sunyaev-Zeldovich Catalogue; by extending the population of the virialized massive galaxy clusters to a population of sources at z>1.5, the PHZ may contain the progenitors of today's clusters. Hence the PHZ opens a new window on the study of the early ages of structure formation, and the understanding of the intensively star-forming phase at high-z.

                    (a)  Z<3 b="" nbsp="" z=""> 4     (c)low-z     (d) high-z.

Q66.  In a composite model of the weak bosons the p-wave bosons are studied. The state with the lowest mass is identified with the boson, which has been observed at the LHC. Specific properties of the excited bosons are studied, in particular their decays into weak bosons and photons. Such decays might have been observed recently with a detector at the Large Hadron Collider and

                      (a)  Bomb      (b) ATLAS    (c) Zetp      (d) Xelyn  

Q67. The surface spin states for bismuth thin films were investigated using a tight-binding model. The model explains the experimental observations using angle-resolved photoemission spectroscopy, including the Fermi surface, the band structure with Rashba spin splitting, and the quantum confinement in the energy band gap of the surface states. A large out-of-plane spin component also appears. The surface states penetrate inside the film to within approximately a few bilayers near the Brillouin-zone center, whereas they reach the center of the film near the Brillouin-zone boundary.

                    (a)  sp^2       (b) sp^4         (c) sp^3       (d)sp^5

 Q68. In this paper, we study the physical meaning of the wave-function of the universe. With the continuity equation derived from the Wheeler-DeWitt (WDW) equation in the mini-super-space model, we show that the quantity ρ(a) = |ψ(a)|^2   for the universe is inversely proportional to the Hubble parameter of the universe. Thus, ρ(a) represents the probability density of the universe staying in  the state a during its evolution, which we call the dynamical interpretation of the wave-function of the universe. We demonstrate that the dynamical interpretation can predict the evolution laws of the universe in the classical limit as those given by the Friedmann equation. Furthermore, we show that the value of the operator ordering factor p in the WDW equation can be determined to be p is equal to

                         (a)     0         (b) -2        (c) -4        (d)  -1

Q69. The universal validity of the second law of thermodynamics is widely attributed to a newly tuned initial condition of the universe. This creates a problem: why is the universe atypical? We suggest that the problem is an artefact created by inappropriate transfer of the traditional concept of entropy to the whole universe. Use of what we call the relational N-body problem as a model indicates the need to employ two distinct entropy-type concepts to describe the universe. One, which we call ‘entaxy’, is novel. It is invariant and decreases as the observable universe evolves. The other is the algebraic sum of the dimension full entropies of branch systems (isolated subsystems of the universe). This conventional additive entropy increases. In our model, the decrease of entaxy is fundamental and makes possible the emergence of branch systems and their increasing entropy. We have previously shown that all solutions of our model divide into two halves at a unique `Janus point' of maximum disorder. This constitutes a common past for two futures each with its own gravitational arrow of time. We now show that these arrows  are expressed through the formation of branch systems within which conventional entropy increases. On either side of the Janus point, this increase is in the same direction in every branch system. We also show that it is only possible to specify unbiased solution-determining data at the Janus point. Special properties of these `mid-point data' make it possible to develop a rational theory of the typicality of universes whose governing law, as in our model, dictates the presence of a Janus point in every solution. If our self-gravitating universe is governed by such a law, then the second law of thermodynamics is a necessary direct consequence of it and does not need any special initial condition.  The entaxy is invariant with.

                  (a) Scale (b) angular momentum (c) energy (d) entropy.

 Q70. Double field theory is an approach for massless modes of string theory, unifying and geometrizing all gauge invariances in manifest O(D, D) covariant manner. In this approach, we derive off-shell conserved Noether current and corresponding Noether potential associated with unified gauge invariances.  We add Wald-type counter two-form to the Noether potential and define conserved global charges as surface integral. We check our O(D, D) covariant formula against various string backgrounds, both geometric and non-geometric. In all cases we examined, we find perfect agreements with previous results. Our formula facilitates to evaluate momenta along not only ordinary space-time directions but also dual space-time directions on equal footing. From this, we confirm recent assertion that null wave in doubled space-time is the same as macroscopic fundamental string in ordinary,  

               (a) Galaxy    (b) Universe   (c) world  (d) space-time

 Q71. The coherent generation of light, from masers to lasers, relies upon the specific structure of the individual emitters that lead to gain. Devices operating as lasers in the few-emitter limit provide opportunities for understanding quantum coherent phenomena, from THz sources to quantum communication. Here we demonstrate a maser that is driven by single electron tunnelling events. Semiconductor double quantum dots (DQDs) serve as a gain medium and are placed inside of a high quality factor microwave cavity. We verify maser action by comparing the statistics of the emitted microwave field above and below the maser,

               (a)  gain    (b) threshold    (c) energy    (d) angular momentum

 Q72. In this work we show that on sub-picosecond time scales optical phonon modes can propagate through the H-bond network of water over relatively long distances (2-4 nm). Using molecular dynamics simulation we find propagating optical phonons in the librational and OH stretching bands. The OH stretching phonon only appears when a polarizable model (TTM3-F) is employed. Both of these phonon modes exhibit LOTO splitting at k = 0, indicating long range dipole-dipole interactions in the system. We study the LOTO splitting as a function of temperature, finding that the splitting increases for the librational mode at higher temperatures but decreases for the stretching mode. Since LO-TO splitting is intimately connected to structure, this analysis opens the door for new insights into how the local structure of water changes with temperature. Our results also explain a previously unnoticed discrepancy one encounters when comparing the librational peaks found in Raman and IR/dielectric spectra. Previously the three Raman peaks at ≈ 435, 600, and 770 cm−¹ were assigned to the twisting, rocking, and wagging librations of single water molecules. Our results indicate these peaks are better understood as a transverse optical phonon, the wagging response of single molecules, and a longitudinal optical phonon. In agreement with the work of Iwano, et. al. (2010) on the librational modes of ice XI, we believe the librational phonons consist of coupled wagging and

                 (a)  rounding       (b) zig-zag     (c) rocking   (d) twisting

Q73. We consider the single-handed spinor field in interaction with its own gravitational field described by the set of field equations given by Weyl field equations written in terms of derivatives that are covariant with respect to the gravitational connection plus Einstein field equations soured with the energy tensor of the spinor: for the Weyl spinor and the ensuing space-time of Weyl-LewisPapapetrou structure, we will find all exact solutions. The solutions are flag-dipole PP-waves in a VSI-space-time, and some of their properties are discussed in view of future,

                  (a) developments  (b) thoughts   (c) ideas   (d) reasons  

Q74. We study the dark matter particle, the dark photon (DP), in the decay of the Higgs-like boson. The nature of dark matter is maintained through the hidden sector including the effects of breaking of the scale invariance. The model is based on the additional U⁰(1) gauge group associated with light DP. The interaction between DP and quarks is mediated by the derivative of the scalar - the dilaton. The latter appears in the conformal sector which triggers the electroweak symmetry breaking. Upper limits are set on the DP mass, the mixing strength between the standard photon and DP. The model does allow to estimate the DP mass with the value of 4.5 MeV. The maximal value of the scale invariance breaking constant is also reported for

               (a) Dark Field  (b) Dark Photon (c) Dark Boson (d) Dark fermion

Q75. In a composite model of the weak bosons the p-wave bosons are studied. The state with the lowest mass is identified with the boson, which has been observed at the LHC. Specific properties of the excited bosons are studied, in particular their decays into weak bosons and photons. Such decays might have been observed recently with the ATLAS detector at the Large Hadron Collider.

            (a)  Quark collider (b) Fermion boost (c) LHC (d) super-collider

Q76. Exotic mesons with hidden strange (ss¯) and heavy quark pairs (QQ¯), where Q = c, b, are considered as diquark-antidiquark systems, (Qs)(Q¯s¯). Taking into account that these states can recombinate into two-meson ones, we study the interplay of these states in terms of the dispersion relation D-function technique. The classification of exotic mesons is discussed, coefficients for decay modes are given, and the predictions for new states are presented. The structure for    ((Qq)(Q¯q¯)),   ((Qs)(Q¯s¯)),  ((Qq) (Q¯s¯))    - states  q = u, d  is a

              (a)  Four-fold      (b) Sixtet        (c) Octet       (d) Nonet

Q77. We investigate dark and visible matter distribution in the Coma cluster in the case of the Navarro-Frenk-White (NFW) profile. A toy model where all galaxies in the cluster are concentrated inside a sphere of an effective radius R_eff is considered. It enables to obtain the mean velocity dispersion as a function of R_eff. We show that, within the observation accuracy of the NFW parameters, the calculated value of R_eff can be rather close to the observable cutoff of the galaxy distribution. Moreover, the comparison of our toy model with the observable data and simulations leads to the following preferable NFW parameters for the Coma cluster: R₂₀₀ ≈ 1.77h⁻¹ Mpc = 2.61Mp.c, c = 3÷4 and M₂₀₀ = 1.29h⁻¹×10¹⁵M_⊙. In the Coma cluster the most of galaxies are concentrated inside a sphere of the effective radius R_eff ∼ 3.7 Mpc and the line-of-sight velocity dispersion is 1004kms⁻¹.

       (a) 1204kms⁻¹  (b) 1040kms⁻¹  (c)  1004kms⁻¹  (d) 1104kms⁻¹      

Q78. In order to observe annihilation and decay of dark matter, several types of potential sources should be considered. Some sources, such as dwarf galaxies, are expected to have very low astrophysical backgrounds but fairly small dark matter densities. Other sources, like the Galactic center, are expected to have larger densities of dark matter but also have more complicated backgrounds from other astrophysical sources. To search for signatures of dark matter, the large field-of-view of the HAWC detector, covering 2sr at a time, especially enables searches from sources of dark matter annihilation and decay, which are extended over several degrees on the sky. With a sensitivity over 2/3 of the sky, HAWC has the ability to probe a large fraction of the sky for the signals of TeV-mass dark matter. In particular, HAWC should be the most sensitive experiment to signals coming from dark matter with masses greater than 10-100 TeV. We present the HAWC sensitivity to annihilating and decaying dark matter signals for several likely sources of these signals of mass of dark matter

          (a) >100TeV  (b) <10tev 100gev="" c="" d="" ev="" nbsp="" o:p="">

Q79. We study the DARK MATER particle, the DARK PHOTON (DP), in the decay of the Higgs-like boson. The nature of dark matter is maintained through the hidden sector including the effects of breaking of the scale invariance. The model is based on the additional U’(1) gauge group associated with light DP. The interaction between DP and quarks is mediated by the derivative of the scalar - the dilaton. The latter appears in the conformal sector which triggers the electroweak symmetry breaking. Upper limits are set on the DP mass, the mixing strength between the standard photon and DP. The model does allow to estimate the DP mass with the value of 4.5 MeV. The maximal value of the scale invariance breaking constant is also

                   (a) Reported (b) observed (c) predicted (d) thought 

Q80. We study theories which naturally select a vacuum with parametrically small Electroweak Scale due to finite temperature effects in the early universe. In particular, there is a scalar with an approximate shift symmetry broken by a technically natural small coupling to the Higgs, and a temperature dependent potential. As the temperature of the universe drops, the scalar follows the minimum of its potential altering the Higgs mass squared parameter. The scalar also has a periodic potential with amplitude proportional to the Higgs expectation value, which traps it in a vacuum with a small Electroweak Scale. The required temperature dependence of the potential can occur through strong coupling effects in a hidden sector that are suppressed at high temperatures. Alternatively, it can be generated perturbatively from a one-loop thermal potential. In both cases, for the scalar to be displaced, a hidden sector must be reheated to temperatures significantly higher than the visible sector. However this does not violate observational constraints provided the hidden sector energy density is transferred to the visible sector without disrupting big bang nucleosynthesis. We also study how the mechanism can be implemented when the visible sector is completed to the Minimal Supersymmetric Standard Model at a high scale. Models with a UV cut-off of 10TeV and no fields taking values over a range greater than 10¹² GeV are possible, although the scalar must have a range of order 10⁸ times the effective decay constant in the periodic part of its

                (a)  perodicity  (b) potential  (c) temperature (d) UV cut-off 

Q81. It is shown that the density of modes of the vibrational spectrum of globular proteins is universal, i.e., regardless of the protein in question it closely follows one universal curve. The present study, including 135 proteins analyzed with a full atomic empirical potential (CHARMM22) and using the full complement of all atoms Cartesian degrees of freedom, goes far beyond confirming previous claims of universality, finding that universality holds even in the high-frequency range (300 – 4000cm⁻¹), where peaks and turns in the density of states are faithfully reproduced from one protein to the next. We also characterize fluctuations of the spectral density from the average, paving the way to a meaningful discussion of rare, unusual spectra and the structural reasons for the deviations in such “outlier” proteins. Since the method used for the derivation of the vibrational modes (potential energy formulation, set of degrees of freedom employed, etc.) has a dramatic effect on the spectral density, another significant implication of our findings is that the universality can provide an exquisite tool for assessing and improving the quality of various models used for NMA computations. Finally, we show that the input configuration too affects the density of modes, thus emphasizing the importance of simplified potential energy formulations that are minimized at the outset.

                        (a)  beginning  (b)  last   (c)outset  (d) inset

82.  A dynamical system framework is used to describe transport processes in plasmas embedded in a magnetic field. For periodic systems with one degree of freedom the Poincar´e map provides a splitting of the phase space into regions where particles have different kinds of motion: periodic, quasi-periodic or chaotic. The boundaries of these regions are transport barriers; i.e., a trajectory cannot cross such boundaries during the whole evolution of the system. Lagrangian Coherent Structure (LCS) generalize this method to systems with the most general time dependence, splitting the phase space into regions with different qualitative behaviours. This leads to the definition of finite-time transport barriers, i.e. trajectories cannot cross the barrier for a finite amount of time. This methodology can be used to identify fast recirculating regions in the dynamical system and to characterize the transport between them. The map is of

                   (a)  Legendre  (b) Poincar’e   (c) Hamilton  (d)Lagrange

Q83.  Unified dark matter models are appealing in that they describe the dark sector in terms of a single component. They however face problems when attempting to account for structure formation: in the linear regime, density fluctuations can become Jeans stable and oscillate rather than collapse, though it is possible that this difficulty may be circumvented by invoking nonlinear clustering. Here we examine the behaviour in the fully nonlinear regime, of collapsed objects that should mimic standard dark matter haloes. It is shown that the pressure gradient associated with the unified dark matter fluid should be significant in the outer parts of galaxies and clusters, and its effects obervable. In this case, no flat or falling rotation curve is possible for any (barotropic) equation of state with associated sound speed decreasing with density (a necessary condition if the fluid is to behave as pressureless matter at high density). The associated density profile is therefore also incompatible with that inferred in the outer part of clusters. For the prototypical case of the generalised Chaplygin gas, it is shown that this limits the values of the equation of state index α that are compatible with observations to α . 0.0001 or α & 2. This is in line from what is deduced from linear analysis. More generally, from the expected properties of dark matter haloes, constraints on the sound speed are derived. For the particular case of the generalised Chaplygin gas, this further constrains the index to α . 10⁻⁹ or α & 6.7. For a unified dark matter fluid to mimic dark halo properties, therefore, it needs to have an equation of state such that the pressure gradients are either minimal or which decrease fast enough so as to be negligible at densities characteristic of the outer parts of

                    (a)  sinks    (b) dips     (c) haloes   (d)   holes

Q84. Spin-2 fields are often candidates in physics beyond the Standard Model namely the models with extra-dimensions where spin-2 Kaluza-Klein gravitons couple to the fields of the SM. Also, in the context of Higgs searches, spin-2 fields have been studied as an alternative to the scalar Higgs boson. In this article, we present the complete three loop QCD radiative corrections to the spin-2 quark-antiquark and spin-2 gluon-gluon form factors in SU(N) gauge theory with n_f light flavors. These form factors contribute to both quark-antiquark and gluon-gluon initiated processes involving spin-2 particle in the hadronic reactions at the LHC. We have studied the structure of infrared singularities in these form factors up to three loop level using Sudakov integro-differential equation and found that the anomalous dimensions originating from soft and collinear regions of the loop integrals coincide with those of the electroweak vector boson and Higgs form factors confirming the universality of the infrared singularities in QCD

                    (a) regularities   (b)systematics  (c) amplitudes (d) notes.

 Q85. LONDON (AP), Scientists and tech experts, including Professor Stephen Hawking and Apple co-founder Steve Wozniak warned Tuesday of a global arms race with weapons using artificial intelligence. In an open letter with hundreds of signatories, the experts argued that if any major military power pushes ahead with development of autonomous weapons, "a global arms race is virtually inevitable, and the endpoint of this technological trajectory is obvious: autonomous weapons will become the Kalashnikovs of "

                      (a) destruction       (b) tomorrow        (c) ester days      (d) fuure

Q86. Windows 10 is coming to PCs and tablets first, but it's also designed to run phones, game consoles and even holographic headsets. It has new features, a streamlined Web browser called Edge and a desktop version of Cortana, the online assistant that is Microsoft's answer to Google Now and Apple's Siri.  Still, the company insists Windows 10 will seem familiar to users of Windows 7, the six-year-old operating system still running on most PCs. Microsoft and PC makers want to erase the memory of the last big update, 2012's Windows 8, which alienated many with its jarring, unwieldy

                (a)  show         (b) design        (c) model           (d) getup

Q87. We propose a new approach to the missing baryons problem. Building on the common assumption that the missing baryons are in the form of the Warm Hot Intergalactic Medium (WHIM), we further assumed here that the galaxy luminosity density can be used as a tracer of the WHIM. The latter assumption is supported by our finding of a significant correlation between the WHIM density and the galaxy luminosity density in the hydrodynamical simulations of Cui et al. (2012). We further found that the fraction of the gas mass in the WHIM phase is substantially (by a factor of ∼1.6) higher within the large scale galactic filaments, i.e. ∼70%, compared to the average in the full simulation volume of ∼0.1 Gpc³. The relation between the WHIM overdensity and the galaxy luminosity overdensity within the galactic filaments is consistent with linear: δ_whim = 0.7 ± 0.1 × δ⁰_LD^.9±0.2.   We applied our procedure to the line of sight to the blazar H2356-309 and found evidence for the WHIM in correspondence of the Sculptor Wall (z ∼0.03 and log N_H = 19.9⁺₋⁰₀^._.3¹) and Pisces-Cetus superclusters (z ∼0.06 and log N_H = 19.7⁺₋⁰₀^._.3²), in agreement with the redshifts and column densities of the X-ray absorbers identified and studied by Fang et al. (2010) and Zappacosta et al. (2010). This agreement indicates that the galaxy luminosity density and galactic filaments are reliable signposts for the WHIM and that our method is robust in estimating the WHIM density. The signal that we detected cannot originate from the halos of the nearby galaxies since they cannot account for the large WHIM column densities that our method and X-ray analysis consistently find in the Sculptor Wall and Pisces-Cetus

               (a) design  (b) clusters (c) superclusters (d) superbugs 

Q88.  The aim of this work is to solve the dispersion relations near the first excitation threshold of photon propagating along the magnetic field in the strong field limit. We have calculated the time damping of the photon in two particular cases: the degenerate gas as well as the diluted gas limit being both important from the Astrophysical point of view. In particular the diluted gas limit could describe the magnethosphere of neutron stars. The solutions have been used to obtain a finite Quantum Faraday angle in both limits. A resonant behavior for the Faraday angle is also obtained. To reproduce the semi-classical result for the Faraday rotation angle the weak field limit is 

            (a) chosen       (b) set      (c) thought      (d)  considered 

Q89. Reproducing the large Earth/Mars mass ratio requires a strong mass depletion in solids within the protoplanetary disk between 1 and 3 AU. The Grand Tack model invokes a specific migration history of the giant planets to remove most of the mass initially beyond 1 AU and to dynamically excite the asteroid belt. However, one could also invoke a steep density gradient created by inward drift and pile-up of small particles induced by gas-drag, as has been proposed to explain the formation of closein super Earths. Here we show that the asteroid belt’s orbital excitation provides a crucial constraint against this scenario for the Solar System. We performed a series of simulations of terrestrial planet formation and asteroid belt evolution starting from disks of planetesimals and planetary embryos with various radial density gradients and including Jupiter and Saturn on nearly circular and coplanar orbits. Disks with shallow density gradients reproduce the dynamical excitation of the asteroid belt by gravitational self-stirring but form Mars analogs significantly more massive than the real planet. In contrast, a disk with a surface density gradient proportional to r^−5.5 reproduces the Earth/Mars mass ratio but leaves the asteroid belt in a dynamical state that is far colder than the real belt. We conclude that no disk profile can simultaneously explain the structure of the terrestrial planets and asteroid belt. The asteroid belt must have been depleted and dynamically excited by a different mechanism such as, for instance, in the Grand Tack

            (a)   Scenario   (b)    outlook    (c) scene   (d) view

Q90.    The FERMI observation of a γ-ray excess from the galactic-centre, as well as the PAMELA, AMS, and AMS-2 anti-proton excesses, and the recent claim of a FERMI γ-ray excess in the Reticulum-2 dwarf galaxy have been used to indicate the possible detection of supersymmetric neutralino dark matter. These are of particular interest as the neutralino annihilation models which fit these observations must have potentially observable consequences across the frequency spectrum, from radio to γ-ray emission. Moreover, since dark matter is expected to be a major matter constituents of cosmic structure, these multi-frequency consequences should be common to structures across the mass spectrum, from dwarf galaxies to galaxy clusters. Thus, in this work we make predictions for the multi-frequency spectra of three well-known sources dominated by dark matter, e.g. the Coma cluster, the galaxy M81, and the Draco dwarf galaxy using models favoured by dark matter interpretations of the aforementioned observations. We pay special attention to the consequences for these models when their cross-sections are renormalised to reproduce the recent γ-ray excess observed in the Reticulum-2 dwarf galaxy, which throw a dark matter interpretation of this excess into doubt. We find that the multi-frequency data of Coma, M81 and Draco disfavour the dark matter interpretation of the AMS, Pamela and Fermi anti-proton excess. However, models derived from FERMI galactic centre observations present no such conflicts, but result in dark matter emissions being sub-dominant in the considered environments, particularly in γ-ray and radio bands. We show that these models can be tested with the upcoming ASTROH mission in the hard X-ray band. Using the sensitivity projections for the Square Kilometre Array, the Cherenkov Telescope Array, as well as the ASTROGAM and ASTRO-H satellites, we determine the detection prospects for a subset of neutralino models that remain consistent with PLANCK cosmological constraints. Although the SKA has the greatest sensitivity to dark matter models, we demonstrate that ASTRO-H is well positioned to probe the X-ray emissions from neutralino annihilation and identify characteristics of the spectra which contain information about the neutralino mass and annihilation channel. This means that multi-frequency observation with the next generation experiments will allow for unprecedented sensitivity to the neutralino parameter space as well as offsetting the individual weaknesses of each observation   

              (a)  outlook       (b)   mode        (c) hype      (d)   list

Q91.  The space weather is extremely mild during solar cycle 24: the number of major geomagnetic storms and high-energy solar energetic particle events are at the lowest since the dawn of the space age. Solar wind measurements at 1 AU using Wind and ACE instruments have shown that there is a significant drop in the density, magnetic field, total pressure, and Alfven speed in the inner heliosphere as a result of the low solar activity. The drop in large space weather events is disproportionately high because the number of energetic coronal mass ejections that cause these events has not decreased significantly. For example, the rate of halo CMEs, which is a good indicator of energetic CMEs, is similar to that in cycle 23, even though the sunspot number has declined by ~40%. The mild space weather seems to be a consequence of the anomalous expansion of CMEs due to the low ambient pressure in the heliosphere. The anomalous expansion results in the dilution of the magnetic contents of CMEs, so the geomagnetic storms are generally weak. CME-driven shocks propagating through the weak heliospheric field are less efficient in accelerating energetic particles, so the particles do not attain high energies. Finally, we would like to point out that extreme events such as the 2012 July 23 CMEs that occurred on the backside of the Sun and did not affect Earth except for a small  

      (a) proton event (b)neutron event (c) helio storm  (d)  quark collusion

Q92. Spiral arms shown by different components may not be spatially coincident, which can constrain formation mechanisms of spiral structure in a galaxy. We reassess the spiral arm tangency directions in the Milky Way through identifying the bump features in the longitude plots of survey data for infrared stars, radio recombination lines (RRLs), star formation sites, CO, high density regions in clouds, and HI. The bump peaks are taken as indications for arm tangencies, which are close to the real density peaks near the spiral arm tangency point but often have ∼ 1^◦ offset to the interior of spiral arms. The arm tangencies identified from the longitudes plots for RRLs, HII regions, methanol masers, CO, high density gas regions, and HI gas appear nearly the same Galactic longitude, and therefore there is no obvious offset for spiral arms traced by different gas components. However, we find obvious displacements of 1.3^◦− 5.8^◦ between gaseous bump peaks from the directions of the maximum density of old stars near the tangencies of the Scutum-Centaurus Arm, the northern part of the Near 3 kpc Arm, and maybe also the Sagittarius Arm. The offsets between the density peaks of gas and old stars for spiral arms are comparable with the arm widths, which is consistent with expectations for quasi-stationary density wave in our

(a)  Gas region      (b) atmosphere      (c)  Galaxy     (d) Universe

Q93. Recent Hubble Space Telescope images have allowed the determination with unprecedented accuracy of motions and changes of shocks within the inner Nebula. These originate from collimated outflows from very young stars, some within the ionized portion of the nebula and others within the host molecular cloud. We have doubled the number of Herbig-Haro objects known within the inner Orion Nebula. We find that the best-known Herbig-Haro shocks originate from a relatively few stars, with the optically visible X-ray source COUP 666 driving many of them. While some isolated shocks are driven by single collimated outflows, many groups of shocks are the result of a single stellar source having jets oriented in multiple directions at similar times. This explains the feature that shocks aligned in opposite directions in the plane of the sky are usually blue shifted because the redshifted outflows pass into the optically thick Photon Dominated Region behind the nebula. There are two regions from which optical outflows originate for which there are no candidate sources in the SIMBAD data base. Shocks measured in inner nebula of

               (a)  Jets    (b) Orion      (c)  Rigs     (d) Constellation

Q94. Context. In the last five years the Fermi Large Area Telescope (LAT) instrument detected GeV gamma-ray emission from five novae. The GeV emission can be interpreted in terms of an inverse Compton process of electrons accelerated in a shock. In this case it is expected that protons in the same conditions can be accelerated to much higher energies. Consequently they may produce a second component in the gamma-ray spectrum at TeV energies. Aims. We aim to explore the very-high-energy domain to search for gamma-ray emission above 50 GeV and to shed light on the acceleration process of leptons and hadrons in nova explosions. Methods. We have performed observations with the MAGIC telescopes of the classical nova V339 Del shortly after the 2013 outburst, triggered by optical and subsequent GeV gamma-ray detections. We also briefly report on VHE observations of the symbiotic nova YY Her and the dwarf nova ASASSN-13ax. We complement the TeV MAGIC observations with the analysis of con- temporaneous Fermi-LAT data of the sources. The TeV and GeV observations are compared in order to evaluate the acceleration parameters for leptons and hadrons. Results. No significant TeV emission was found from the studied sources. We computed upper limits on the spectrum and night-by-night flux. The combined GeV and TeV observations of V339 Del limit the ratio of proton to electron luminosities to Lp

                     (a)  <~0.15 (b)   >-0.15     (c)   = -0.15    (d)  -.20

Q95. We use photometric and spectroscopic observations of the detached eclipsing binaries V40 and V41 in the globular cluster NGC 6362 to derive masses, radii, and luminosities of the component stars. The orbital periods of these systems are 5.30 and 17.89 d, respectively. The measured masses of the primary and secondary components (M_p, M_s) are (0.8337±0.0063, 0.7947±0.0048) M_⊙ for V40 and (0.8215±0.0058, 0.7280±0.0047) M_⊙ for V41. The measured radii (R_p, R_s) are (1.3253±0.0075, 0.997±0.013) R_⊙ for V40 and (1.0739±0.0048, 0.7307±0.0046) R_⊙ for V41. Based on the derived luminosities, we find that the distance modulus of the cluster is 14.74±0.04 mag – in good agreement with 14.72 mag obtained from CMD fitting. We compare the absolute parameters of component stars with theoretical isochrones in mass-radius and mass-luminosity diagrams. For assumed abundances [Fe/H] = -1.07, [α/Fe] = 0.4, and Y = 0.25 we find the most probable age of V40 to be 11.7±0.2 Gyr, compatible with the age of the cluster derived from CMD fitting (12.5±0.5 Gyr). V41 seems to be markedly younger than V40. If independently confirmed, this result will suggest that V41 belongs to the younger of the two stellar populations recently discovered in NGC 6362. The orbits of both systems are eccentric. Given the orbital period and age of V40, its orbit should have been tidally circularized some ∼7 Gyr ago. The observed eccentricity is most likely the result of a relatively recent close stellar

             (a) outburst       (b)  dissipation     (c)  encounter    (d) collision

Q96. Milli-second pulsars (MSPs) are rapidly spinning neutron stars, with spin periods P_s . 10 ms, which have been most likely spun up after a phase of matter accretion from a companion star. In this work we present the results of the search for the companion stars of four binary milli-second pulsars, carried out with archival data from the Gemini South telescope. Based upon a very good positional coincidence with the pulsar radio coordinates, we likely identified the companion stars to three MSPs, namely PSR J0614−3329 (g=21.95±0.05), J1231−1411 (g=25.40±0.23), and J2017+0603 (g=24.72±0.28). For the last pulsar (PSR J0613−0200) the identification was hampered by the presence of a bright star (g=16±0.03) at ∼2^′′ from the pulsar radio coordinates and we could only set 3σ upper limits of g = 25.0, r = 24.3, and i = 24.2 on the magnitudes of its companion star. The candidate companion stars to PSR J0614−3329, J1231−1411, and J2017+0603 can be tentatively identified as He white dwarfs (WDs) on the basis of their optical colours and brightness and the comparison with stellar model tracks. From the comparison of our multi-band photometry with stellar model tracks we also obtained possible ranges on the mass, temperature, and gravity of the candidate WD companions to these three MSPs. Optical spectroscopy observations are needed to confirm their possible classification as He WDs and accurately measure their stellar,

                (a) parameters       (b) orbitals      (c) roots      (d) flangs

Q97. The nearby active galaxy IC310, located in the outskirts of the Perseus cluster of galaxies is a bright and variable multi-wavelength emitter from the radio regime up to very high gamma-ray energies above 100GeV. Originally, the nucleus of IC310 has been classified as a radio galaxy. However, studies of the multi-wavelength emission showed several properties similarly to those found from blazars as well as radio galaxies. In late 2012, we have organized the first contemporaneous multi-wavelength campaign including radio, optical, X-ray and gamma-ray instruments. During this campaign an exceptionally bright flare of IC310 was detected with the MAGIC telescopes in November 2012 reaching an averaged flux level in the night of up to one Crab above 1TeV with a hard spectrum over two decades in energy. The intra-night light curve showed a series of strong outbursts with flux-doublingtime scales as fast as a few minutes. The fast variability constrains the size of the gamma-ray emission regime to be smaller than 20% of the gravitational radius of its central black hole. This challenges the shock acceleration models, commonly used to explain gamma-ray radiation from active galaxies. Here, we will present more details on the MAGIC data and discuss several possible alternative emission,

                (a) events      (b) models      (c) criteria       (d) possibilities

Q98. Pair cascades from millisecond pulsars (MSPs) may be a primary source of Galactic electrons and positrons that contribute to the increase in positron flux above 10 GeV as observed by PAMELA and AMS−02. The Fermi Large Area Telescope (LAT) has increased the number of detected Gamma-ray MSPs tremendously. Light curve modelling further more favours abundant pair production in MSP magnetospheres, so that models of primary cosmic-ray positrons from pulsars should include the contribution from the larger numbers of MSPs and their potentially higher positron output per source. We model the contribution of Galactic MSPs to the terrestrial cosmic-ray electron / positron flux by using a population synthesis code to predict the source properties of present day MSPs. We simulate pair spectra assuming an offset-dipole magnetic field which boosts pair creation rates. We also consider positrons and electrons that have additionally been accelerated to very high energies in the strong intra-binary shocks in black widow (BW) and red-back (RB) binary systems. We transport these particles to Earth by calculating their diffusion and the radiative energy losses they suffer in the Galaxy using a model. Our model particle flux increases for nonzero offsets of the magnetic polar caps. We find that pair cascades from MSP magnetospheres contribute only modestly around a few tens of GeV to the measured fluxes. BW and RB fluxes may reach a few tens of percent of the observed flux up to a few TeV. Future observations should constrain the source properties in this

                  (a)  section         (b) value      (c)  case     (d) range

Q99. Recent experiments on certain Fe-based superconductors have hinted at a role for paired electrons in "incipient" bands that are close to, but do not cross the Fermi level. Related theoretical works disagree on whether or not strong-coupling superconductivity is required to explain such effects, and whether a critical interaction strength exists. In this work, we consider various versions of the model problem of pairing of electrons in the presence of an incipient band, within a simple multiband weak-coupling BCS approximation. We categorize the problem into two cases: case (1) where superconductivity arises from the "incipient band pairing" alone, and case (2) where it is induced on an incipient band by pairing due to Fermi-surface based interactions. Negative conclusions regarding the importance of incipient bands have been drawn so far largely based on case(1), but we show explicitly that models under case(II) are qualitatively different, and can explain the non-exponential suppression of Tc, as well as robust large gaps on an incipient band. In the latter situation, large gaps on the incipient band do not require a critical interaction strength. We also model the interplay between phonon and spin fluctuation driven superconductivity and describe the bootstrap of electron-phonon superconductivity by spin fluctuations coupling the incipient and the regular bands. Finally, we discuss the effect of the dimensionality of the incipient band on our results. We argue that pairing on incipient bands may be significant and important in several Fe-based materials, including LiFeAs, FeSe intercalates and FeSe monolayers on strontium titanate, and indeed may contribute to high critical

              (a) magnitudes      (b) values     (c) ranges      (d) temperatures

Q100. Cavity quantum electrodynamics (CQED) plays an elegant role of studying strong coupling between light and matter. However, a non-mechanical, direct and dynamical control of the used mirrors is still unavailable. Here we theoretically investigate a novel type of dynamically controllable cavity composed of two atomic mirrors. Based on the electromagnetically induced transparency (EIT), the reflectance of atomic mirror is highly controllable through its dispersive properties by varying the intensity of applied coupling fields or the optical depth of atomic media. To demonstrate the uniqueness of the present cavity, we further show the possibility of manipulating vacuum-induced diffraction of a binary Bose-Einstein condensate (BEC) when loading it into a dispersive cavity and experiencing super-radiant scatterings. Our results may provide a novel all-optical element for atom optics and shine new light on controlling light-matter

             (a) boosts       (b) interaction     (c) collisions     (d) efforts

Q101. We have proposed to create  modes along the vortex lines of Dirac mass in Weyl materials. Compared to the helical dislocation modes in weak topological insulators, our unidirectional modes are completely robust in the sense that they are immune to any kind of backscattering, therefore, they are able to support dissipationless transport inside the 3D bulk. In this respect our proposal is of significant practical use. Our proposal is especially feasible in the photonic Weyl materials, for which it is convenient to design and manipulate the Dirac mass. On the theoretical side, our result sheds some light on the topological θ term. Earlier Reference a Chern-Simons form has been found for θ, which is defined in terms of the bulk quantities. A vortex line of θ is an axion-string. In our model the bulk systems (I, II, III, IV) are indistinguishable from each other, thus it is pointless to define here the precise value of θ from the bulk, however, relative θ angles seem well-defined. Finally, we remark that our proposal may be generalized to other topological materials (e.g. topological phononic or acoustic materials). The modes along vortex lines are,

      (a) unidirectional  (b) omnipresent  (c) irregular (d) dissipative

Q102. We study numerically the detailed structure and decay dynamics of isolated monopoles in conditions similar to those of their recent experimental discovery. We find that the core of a monopole in the polar phase of a spin-1 Bose–Einstein condensate contains a small half-quantum vortex ring. Well after the creation of the monopole, we observe a dynamical quantum phase transition that destroys the polar phase. Strikingly, the resulting ferromagnetic order parameter exhibits a Dirac monopole in its synthetic magnetic field. Our numerical studies suggest that the isolated monopole structure observed in Ref. [M. W. Ray, E. Ruokokoski, K. Tiurev, M. Mo¨tt¨onen, and D. S. Hall, unpublished (2015)] contains a small Alice ring [Ruostekoski and J. R. Anglin, Phy. Rev. Lett. 91,190402, 2003. This vortex ring is destroyed by a subsequent dynamical phase transition into a ferromagnetic order parameter supporting a Dirac monopole. Although the quadrupole field has been observed to stabilize the polar phase of a ⁸⁷Rb condensate if the field zero is well outside the condensate, our simulations reveal that after the field zero is brought into the condensate, the polar phase decomposes on a time scale of 100ms. We attribute this behaviour to the spatially varying magnetic field and the linear Zeeman interaction. Neither the spin–spin interactions, quadratic Zeeman effect nor three-body recombination have a significant effect on the decay dynamics. However, the strength of the magnetic field gradient is shown to have a detrimental effect on the decay speed and characteristics. These studies set the stage for the detailed dynamics of topological point defects in quantum fields. Finding ways to extend the lifetime of the defect further and thereafter to study the dynamics of multiple interacting point defects remain for future

              (a) thoughts  (b) trials (c) discussions (d) challenges

Q103. In high-performance solar cells based on polymeric semiconductors, the mechanism of photo-carrier generation on <100-fs 2d="" a="" and="" be="" between="" can="" chains="" charge-transfer="" coherent="" correlations:="" correlations="" coupling="" detailed="" develop="" dynamics="" early-time="" electronic="" excitation="" excitons="" in="" interpret="" investigated="" involved="" is="" light="" measure="" measurements="" measures="" need="" nonlinear="" novel="" of="" off-diagonal="" on="" order="" particular="" photocurrent="" picture="" polymer="" predictions.="" preliminary="" presented="" proceeding="" processes="" production.="" recent="" report="" span="" spectral="" spectroscopic="" spectroscopy.="" spectroscopy="" spectrum.="" states="" such="" technique="" that="" the="" theoretical="" these="" this="" timescales="" to="" two-dimensional="" ultrafast="" unravelled.="" using="" we="" work="" yet=""> photocurrent excitation spectra measured on polymer-based solar cell. Our data show how this novel technique can be applied in the investigation of the charge photogeneration process in such systems. The unique added value of this new experimental method stems from the possibility to directly probe the final observable of interest, i.e. photocurrent, for the understanding of the mechanism of primary charge generation in organic solar cells in their operating 

                         (a) limits        (b) threshold      (c) space         (d) regime

Q104.  Searches for dark matter imprints are one of the most active areas of current research. We focus here on light fields with mass m_B, such as axions and axion-like candidates. Using perturbative techniques and full-blown nonlinear Numerical Relativity methods, we show that (i) dark matter can pile up in the center of stars, leading to configurations and geometries oscillating with frequency which is a multiple of f=2.5x10E+14 m_B.c²/eV Hz. These configurations are stable throughout most of the parameter space, and arise out of credible mechanisms for dark-matter capture. Stars with bosonic cores may also develop in other theories with effective mass couplings, such as (massless) scalar-tensor theories. We also show that (ii) collapse of the host star to a black hole is avoided by efficient gravitational cooling mechanisms. Previous works on the subject of DM accretion by stars have implicitly assumed that the DM core is able to grow without bound and eventually collapse to BHs. Our results, from full nonlinear simulations of the field equations, show that the core may stop growing when it reaches a peak value, at the threshold of stability, if DM is composed of light massive fields. Gravitational cooling quenches the core growth for massive cores and the core growth halts, close to the

         (a) peak value  (b) limit value  (c) maximum value  (d) minimum value.

Q105.  We investigate a spatially flat Friedmann-Robertson-Walker (FRW) scenario with two interacting components, dark matter and variable vacuum energy (VVE) densities, plus two decoupled components, one is a baryon term while the other behaves as a radiation component. We consider a linear interaction in the derivative dark component density. We apply the χ² method to the observational Hubble data for constraining the cosmological parameters and analyze the amount of dark energy in the radiation era for the model. It turns out that our model fulfills the severe bound of Ω_x(z ' 1100) < 0.009 at 2σ level, so is consistent with the recent analysis that include cosmic microwave background anisotropy measurements from Planck survey, the future constraints achievable by Euclid and CMBPol experiments, reported for the behaviour of the dark energy at early times, and fulfils the stringent bound Ω_x(z'10¹⁰)<0 i="">.

04 at 2σ level in the big-bang nucleosynthesis epoch. We also examine the cosmic age problem at high redshift associated with the old quasar APM 08279+5255 and estimate the age of the universe

             (a)  aeons ago  (b) today (c) future (d) past

 Q106. In this work a cosmological scenario where dark matter interacts with a variable vacuum energy for a spatially flat Friedman- Robertson- Walker space-time is analysed. One of the aims is to show how a particular interaction in the dark sector can be used to get a model of Emergent Universe. After that we analyse the viability  of two particular models by taking account recent observations. The updated observational Hubble data is used in order to constrain the cosmological parameters of the models and the amount of dark energy in the radiation era is estimated. It is shown that the two models fulfil the severe bounds of   Ωx(z~1100)  

           (a) <0 .0009="" b="" c="" d="" nbsp=""> 0.009    

Q107. We construct a 2+1 dimensional model that sustains superconductivity at all temperatures. This is achieved by introducing a Chern Simons mixing term between two Abelian gauge fields A and Z. The superfluid is described by a complex scalar charged under Z, whereas a sufficiently strong magnetic field of A forces the superconducting condensate to form at all temperatures. In fact, at finite temperature, the theory exhibits Berezinsky-Kosterlitz-Thouless phase transition due to proliferation of topological vortices admitted by our construction. However, the critical temperature is proportional to the magnetic field of A, and thus, the phase transition can be postponed to high temperatures by increasing the strength of the magnetic field. This model can be a step towards realizing the long sought room temperature

(a) fluidity  (b) superfluidity  (c)superconductivity (d) conductivity

Q108. The Miniature X-ray Solar Spectrometer (MinXSS) is a 3-Unit (3U) CubeSat developed at the Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado, Boulder (CU). Over 40 students contributed to the project with professional mentorship and technical contributions from professors in the Aerospace Engineering Sciences Department at CU and from LASP scientists and engineers. The scientific objective of MinXSS is to study processes in the dynamic Sun, from quiet-Sun to solar flares, and to further understand how these changes in the Sun influence the Earth’s atmosphere by providing unique spectral measurements of solar soft x-rays (SXRs). The enabling technology providing the advanced solar SXR spectral measurements is the Amptek X123, a commercial-off-the-shelf (COTS) silicon drift detector (SDD). The Amptek X123 has a low mass (~324 g after modification), modest power consumption (~2.5 W), and small volume (2.7” x 3.9” x 1.0”), making it ideal for a CubeSat. This paper provides an overview of the MinXSS mission: the science objectives, project history, subsystems, and lessons learned that can be useful for the small-satellite

(a) community  (b) region    (c) township     (d) activity

Q109.  We revisit the calculation of dark matter relic abundances in scalar-tensor gravity using a generic form A(ϕ_∗) = e^βϕ2∗/2 for the coupling between the scalar field ϕ_∗ and the metric, for which detailed Big Bang Nucleosynthesis constraints are available. We find that BBN constraints restrict the modified expansion rate in these models to be almost degenerate with the standard expansion history at the time of dark matter decoupling. In this case the maximum level of enhancement of the dark matter relic density was found to be a factor of ∼ 3, several orders of magnitude below that found in previous investigations. The inherent attraction mechanism exhibited by many scalar-tensor gravity models towards General Relativity allows for deviations from the standard cosmological scenario in the early universe that may not show up in present observational data. In fact, it has been conjectured that relic abundance calculations may be one of the few probes capable of discriminating the predictions of scalar-tensor scenarios from standard General Relativity. To find out, we determined the evolution of the coupled scalar field from first principles, allowing us to calculate the modified expansion rate in the scalar-tensor gravity scenario, which we then used to calculate the dark matter relic abundance. As a specific example we considered the prototypical quadratic coupling A(φ_*)= exp (½ β φ_*²) and found that the maximum enhancement for a m_χ = 100 GeV WIMP was

Ω_DM^ST/Ω_DM^GR ~ 3.  Although this ratio would increase with increasing WIMP mass, the level of enhancement is still far below that found in previous relic abundance investigations in scalar-tensor

(a)  prediction   (b) prediction  (c) theory  (d) cosmology

Q110. We show numerically that the ‘deconfined’ quantum critical point between the N´eel antiferromagnet and the columnar valence–bond–solid, for a square lattice of spin-1/2s, has an emergent SO(5) symmetry. This symmetry allows the N´eel vector and the valence-bond-solid order parameter to be rotated into each other. It is a remarkable 2+1–dimensional analogue of the SO(4) = [SU(2) × SU(2)]/Z₂ symmetry that appears in the scaling limit for the spin–1/2 Heisenberg chain. The emergent SO(5) is strong evidence that the phase transition in the 2+1D system is truly continuous, despite the violations of finite-size scaling observed previously in this problem. It also implies surprising relations between correlation functions at the transition. The symmetry enhancement is expected to apply generally to the critical two-component Abelian Higgs model (noncompact CP¹ model). The result indicates that in three dimensions there is an SO(5)-symmetric conformal field theory which has no relevant singlet operators, so is radically different to conventional  Wilson-Fisher-type conformal field 

(a) theories (b) findings (c) results (d) predictions

Q111. The equivalent width of the SiO band at 8 µm increases as the stars grow cooler, but it increases more gradually at later spectral classes. The scatter is considerable and intrinsic to the sample. These results confirm the earlier study by Heras et al. (2002). The scatter does not result from differences in the luminosities or variability properties of the stars. Our synthetic spectra confirm that the structure in our spectra between 6.3 and 7.5 µm is from H₂O absorption. These bands are not easily detected in the K giants, but in the M giants, they increase in strength as the stars grow cooler, but again, with considerable scatter. In this case, the scatter arises from the variability properties of the stars, with more variable sources generally showing stronger absorption in a given spectral class. The OH bands at 14–17 µm climb in strength from K0 to K5, but for cooler stars show little obvious dependence on temperature. The scatter in equivalent widths in the M giants is considerable. Variability plays no obvious role on OH band

(a)  Extension (b) length (c)strength (d) force

Q112.  The newly reported observations were made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. NASA provided support of this work through contract 1257184 issued by JPL/Caltech. We thank the science editor, D. Gies, and the anonymous referee, whose input led to a much improved paper, and G. van Belle, whose comments helped us better utilize the photometry. This research has made use of NASA’s Astrophysics Data System and the SIMBAD database, which is operated at Centre de Donn´ees astronomiques in Strasbourg, France. The Infrared Science Archive (IRSA) at Caltech has also proven to be extremely helpful.  We observed a sample of 20 M giants with the Infrared Spectrograph on the Spitzer Space Telescope. Most show absorption structure at 6.6–6.8 µm which we identify as water vapour, and in some cases, the absorption extends from 6.4 µm into the SiO band at 7.5 µm. Variable stars show stronger H₂O absorption. While the strength of the SiO fundamental at 8 µm increases monotonically from spectral class K0 to K5, the dependence on spectral class weakens in the M giants. As with previously studied samples, the M giants show considerable scatter in SiO band strength within a given spectral class. All of the stars in our sample also show OH band absorption, most noticeably in the 14–17 µm region. The OH bands behave much like the SiO bands, increasing in strength in the K giants but showing weaker dependence on spectral class in the M giants, and with considerable scatter. An examination of the photometric properties reveals that the V − K colour may be a better indicator of molecular band strength than the spectral class. The transformation from Tycho colours to Johnson B −V colour is double-valued, and neither B −V nor BT − VT colour increases monotonically with spectral class in the M giants like they do in the K giants. Finally, since the attraction mechanism towards GR is typically initiated prior to dark matter freeze-out so that the effect on the dark matter relic abundance is only modest, the scalar-tensor scenario with a quadratic coupling to matter does not provide a significantly different picture from the standard cosmological scenario. Hence, we conclude that unless reasonably precise details about the nature of the dark matter particle and its interactions are known, relic abundance calculations are most likely unable to discriminate scalar-tensor gravity from General 

(a)  Relativity (b) Theory (c) predictions (d) enumeration

Q113. Solar active region (AR) 11283 is a very magnetically complex region and it has produced many eruptions. However, there exists a non-eruptive filament in the plage region just next to an eruptive one in the AR, which gives us an opportunity to perform a comparison analysis of these two filaments. The coronal magnetic field extrapolated using a CESE–MHD–NLFFF code (Jiang & Feng 2013) reveals that two magnetic flux ropes (MFRs) exist in the same extrapolation box supporting these two filaments, respectively. Analysis of the magnetic field shows that the eruptive MFR contains a baldpatch separatrix surface (BPSS) co-spatial very well with a pre-eruptive EUV sigmoid, which is consistent with the BPSS model for coronal sigmoids. The magnetic dips of the non-eruptive MFRs match Hα observation of the non-eruptive filament strikingly well, which strongly supports the MFR-dip model for filaments. Compared with the non-eruptive MFR/filament (with a length of about 200 Mm), the eruptive MFR/filament is much smaller (with a length of about 20 Mm), but it contains most of the magnetic free energy in the extrapolation box and holds a much higher free energy density than the non-eruptive one. Both the MFRs are weakly twisted and cannot trigger kink instability. The AR eruptive MFR is unstable because its axis reaches above a critical height for torus instability, at which the overlying closed arcades can no longer confine the MFR stably. On the contrary, the quiescent MFR is very firmly held by its overlying field, as its axis apex is far below the torus-instability threshold height. Overall, this comparison investigation supports that MFR can exist prior to eruption and the ideal MHD instability can trigger MFR

                 (a) criticality (b) erosion  (c) eruption   (d) disruption

 

Q114. A macronova (or kilonova) was observed as an infrared excess several days after short gamma-ray burst, GRB 130603B. Although the r-process radioactivity is widely discussed as an energy source, it requires huge mass of ejecta from a neutron star (NS) pose that the X-ray excess simultaneously observed with the infrared excess can naturally heat the ejecta, leading to the thermal re-emission as observed in infrared. This X-ray-powered model explains both the X-ray and infrared excesses with a single energy source by the central engine like a black hole, and allows for broader parameter region, in particular smaller ejecta mass ∼ 10⁻³ − 10⁻²M_⊙  with iron mixed as suggested by general relativistic simulations for typical NS-NS mergers, than the previous models. We also discuss the other macronova candidates in GRB 060614 and GRB 080503, and implications for the search of electromagnetic counterparts to gravitational

(a)  Disturbance (b) effects (c) influence (d) waves.   

Q115. For metrology, geodesy and gravimetry in space, satellite based instruments and measurement techniques are used and the orbits of the satellites as well as possible deviations between nearby ones are of central interest. The measurement of this deviation itself gives insight into the underlying structure of the space-time geometry, which is curved and therefore described by the theory of general relativity (GR). In the context of GR, the deviation of nearby geodesics can be described by the Jacobi equation that is a result of linearizing the geodesic equation around a known reference geodesic with respect to the deviation vector and the relative velocity. We review the derivation of this Jacobi equation and restrict ourselves to the simple case of the space-time outside a spherically symmetric mass distribution and circular reference geodesics to find solutions by projecting the Jacobi equation on a parallel propagated tetrad as done by Fuchs. Using his results, we construct solutions of the Jacobi equation for different physical initial scenarios inspired by satellite gravimetry missions and give a set of parameter together with their precise impact on satellite orbit deviation. We further consider the Newtonian analog and construct the full solution that exhibits a similar structure, within this

(a)   construct  (b) conjecture (c) formalism (d) theory

Q116. The Crab Nebula is the brightest source in the very-high-energy (VHE) gamma-ray sky and one of the best studied non-thermal objects. The dominant VHE emission mechanism is believed to be inverse Compton scattering of low energy photons on relativistic electrons. While it is unclear how the electrons in the nebula are accelerated to energies of 10¹⁶ eV, it is general consensus that the ultimate source of energy is the Crab pulsar at the center of the nebula. Studying VHE gamma-ray emission provides valuable insight into the emission mechanisms and ultimately helps to understand the remaining mysteries of the Crab, for example, how the Poynting dominated energy flow is converted into a particle dominated flow of energy. We report on the results of six years of Crab observations with VERITAS comprising 115 hours of data taken between 2007 and 2013. VERITAS is an array of four 12-meter imaging air Cherenkov telescopes located in southern Arizona. We report on the energy spectrum, light curve, and a study of the VHE extension of the Crab Nebula in the Gamma Ray

                 (a) Domain    (b) Sky      (c) Ocean     (d) Plains

 

===================================================================================================================================================

Answers

Q1.a. Q2.a. Q3.a. Q4. a. Q5.c. Q6.a. Q7.b. Q8.a. Q9.b. Q10.c. Q11.a.  Q12.d.   Q13.a. Q14.a. Q15.b. Q16.a. Q17.d. Q18.b.  Q19.c. Q20.a. Q21.b. Q.22.a. Q.23.c. Q.24.c. Q.25.c. Q26.c. Q27.a. Q28.a. Q29.a. Q30.c. Q31.a. Q32.a. Q33.d. Q34.a. Q35.a. Q36.b. Q37.a. Q38.a. Q39.a Q40.b. Q41.a. Q42.c. Q43.d. Q44.a. Q.45.c. Q.46.b. Q.47.b. Q48.c. Q.49.a Q50.c. Q51.c. Q52.a. Q53.a. Q54.c.   Q55.d. Q56.a. Q57.a. Q58.b. Q59.b. Q60.c. Q61.c Q62.b. Q63.b. Q64.c. Q65. Q66.b. Q67.c. Q68.b. Q69.a. Q70.d. Q71.b. Q72.c. Q73.a. Q74.b. Q75.c. Q76.d. Q77.c. Q78.a. Q79.a. Q80.b. Q81.c. Q82.b. Q83.c. Q84.c. Q85.b. Q86.b. Q87.c. Q88.d. Q89.a. Q90.b. Q91.a.  Q92.c. Q93.b. Q94.a. Q95.c. Q96.a. Q97.b. Q98.c. Q99.d. Q100.b. Q101.a. Q102.d. Q103.d. Q104.a. Q105.b. Q106.c. Q107.c. Q108.a. Q109.d. Q110.a. Q111.c. Q112.c. Q113.c.  Q114.d. Q115.d.  Q116.b.