DOCSLIB.ORG

String Theory, QCD and Black Holes

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
String Theory, QCD and Black Holes Black Hole Microstate Structure Fuzzballs and Firewalls Iosif Bena IPhT, CEAEA Saclay with Nick Warner, Jan deBoer, Micha Berkooz, Simon Ross, Gianguido Dall’Agata, Stefano Giusto, Masaki Shigemori, Dieter van den Bleeken, Monica Guica, Sheer El-Showk, Stanislav Kuperstein, Hagen Triendl, Bert Vercnocke, Andrea Puhm, Ref. Ares(2012)790792 - 29/06/2012 ! Department C "Grant Management" ! Mittwoch, 12. März 2014 ! Subject: Aggressive marketing from publishing houses Dear Madam, Dear Sir, The European Research Council Executive Agency (ERCEA) would like to alert you of publishing houses and online publications which try to make profit out of publishing articles, or interviewing researchers funded from the EU budget, either by the European Research Council (ERC) or by the European Commission (EC). From time to time participants in projects funded under the EU framework programmes are contacted – often by telephone - by organisations seeking payment in return for publishing information on the work being undertaken within their projects. As with "cold calling" in general, the claims and assertions made should be treated with an appropriate level of caution before a decision is made on the best course of action. These publications and their services have not been endorsed by the EC, or the ERCEA. Common tactics to secure business may include vague references to high-level contributions from decision makers, or making the project participant believe that his or her activities have been identified on the basis of special merit which may not be the case. Commercial entities use many ways of promoting their services, but grant-holders are not obliged to use them. Whatever the impression given by such service providers, their products have not received any formal approval or endorsement from the EC or the ERCEA. Beneficiaries and their Principal Investigators are free to decide which types of external services are needed; the costs of such services are eligible as long as they meet the conditions set out in the annexes of their grant agreement. If you need further advice on this matter please contact !"#$#%&'()'*+,-.)'* If you as an ERC Principal Investigator or your Host Institution have been or would in the future be subject to these practices, it would be much appreciated if you could inform the ERCEA grant management services at your earliest convenience (same email address as above). Thank you for attention. Yours sincerely, [Signed] Mechtild May Head of Department C a.i. Black Holes Bekenstein & Hawking: Behave like thermodynamic objects Temperature, entropy: S ~ 10 77 solar mass BH S ~ 10 90 BH at center of Milky Way Mittwoch, 12. März 2014 Black Holes Bekenstein & Hawking: Behave like thermodynamic objects Temperature, entropy: S ~ 10 77 solar mass BH S ~ 10 90 BH at center of Milky Way Quantum 10 90 10000000 … 00000 Mechanics: e = e states Mittwoch, 12. März 2014 Black Holes Bekenstein & Hawking: Behave like thermodynamic objects Temperature, entropy: S ~ 10 77 solar mass BH S ~ 10 90 BH at center of Milky Way Quantum 10 90 10000000 … 00000 Mechanics: e = e states General HAIR Relativity: 1 big fat state Information paradox Mittwoch, 12. März 2014 WHERE ARE THE STATES ??? HOW DO THEY LOOK ??? • Very hard question – Quantum Gravity • Simpler question: – Count black hole states in any other way ? Strominger and Vafa (1996) + 1792 other articles Strings and Black Hole Branes Finite Gravity Zero Gravity Mittwoch, 12. März 2014 Ø Count quantum states at zero gravity Ø Entropy matches black hole classical horizon area !!! Ø 2 absolutely different calculations (Cardy Formula vs. classical area) Ø Amazing success Ø Modular forms, hypergeometric, other beasts Ø Unmatched in other theories of gravity String-QCD-BH STATISTICAL CFT ENSEMBLE STATES MECHANICS (Boundary) another way STROMINGER ! VAFA FILLPRESENT to understand: ENTROPY MATCHING WORK AdS-CFT GEOMETRIES Gravity BLACK HOLE Correspondence WITH NO HORIZON (Bulk) FigureMittwoch, 1: 12. MärzAn 2014 illustrative description of this picture of black holes. My research focuses on con- structing more microstate geometries with no horizon, and on improving the dictionary between the existing ones and the states of the CFT (the dashed vertical arrow). paradox: microstates have unitary physics, and thus information is not lost. Second, since the maximal entropy in a region of space comes from microstates that have the same size as the would-be black hole, this would prove ’t Hooft’s holographic principle. Third, these microstates will appear whenever we have a large-enough energy density, and it is quite likely that their physics will be dominant in cosmological settings, like in the Big Bang and the Big Crunch singularities. To use an analogy from classical physics, one can say this picture could revolutionize quantum gravity and the physics of black holes in the same way in which statistical physics revolutionized the understanding of thermodynamics. Furthermore, this picture of black holes might also be experimentally testable with the gravity wave detector LISA or if black holes are found at the Large Hadron Collider. It is therefore a crucial problem in quantum gravity to establish whether this picture is correct. In previous work I have taken quite a few important steps in this direction by constructing and analyzing huge families of black hole microstates, both in string theory and in supergravity. In the future, I believe there are two directions in this research programme that both have a good shot at proving or disproving this revolutionary picture of black holes. The first is to construct a precise map between the states of the dual boundary theory and the solutions we have constructed. Per Kraus and I have been the first to describe black rings in this CFT, and I believe I have some, and I can master the other tools needed to successfully attack this problem. Once this map is obtained, I intend to find the bulk geometries that correspond to the typical states of the CFT. These geometries would be then the typical microstates of the black hole; if they are horizonless, this would give a proof that the black hole is a thermodynamic description of an ensemble of horizonless configurations. The second direction is to construct more generic three-charge solutions, that have black hole charges and depend on several continuous functions. The solutions N. Warner and I have constructed have the appropriate charges, but do not depend on arbitrary functions. Other groups (including my present postdoc, A. Saxena) have on the other hand constructed solutions that depend on arbitrary functions, but do not have black hole charges. I think our methods can be combined to build these more generic solutions. We can then count them and see if they can account for the entropy of the black hole. If they do, this would again establish that black holes are ensembles of horizonless configurations. Another direction that is important to pursue in longer term is the construction of mi- crostates of near-BPS and non-BPS black holes. Most of the effort in this field has so far concentrated on constructing and analyzing microstates of BPS (supersymmetric) black holes. This is enough for the purpose of establishing this picture of black holes: if one can prove that BPS black holes are ensembles of horizonless microstates, then it will be rather unlikely that non-BPS black holes will not have the same description. However, if one is to use this picture Strominger and Vafa (1996): Count Black Hole Microstates (branes + strings) Correctly match B.H. entropy !!! Zero Gravity Black hole regime of parameters: Standard lore: As gravity becomes stronger, - brane configuration becomes smaller - horizon develops and engulfs it Susskind Horowitz, Polchinski - recover standard black hole Damour, Veneziano Mittwoch, 12. März 2014 Strominger and Vafa (1996): Count Black Hole Microstates (branes + strings) Correctly match B.H. entropy !!! Zero Gravity Black hole regime of parameters: Identical to black hole far away. Horizon → Smooth cap Giusto, Mathur, Saxena Bena, Warner Berglund, Gimon, Levi Mittwoch, 12. März 2014 BIG QUESTION: Are all black hole microstates becoming geometries with no horizon ? ? Black hole = ensemble of horizonless microstates Mathur & friends Mittwoch, 12. März 2014 Analogy with ideal gas Thermodynamics Statistical Physics (Air = ideal gas) (Air -- molecules) S P V = n R T e microstates dE = T dS + P dV typical atypical Thermodynamics Statistical Physics Black Hole Solution Microstate geometries Long distance physics Physics at horizon Gravitational lensing Information loss Mittwoch, 12. März 2014 Other formulations: e.g. Bena, Warner, 2007 - Thermodynamics (EF T) breaks down at horizon. New low-mass d.o.f. kick in. - No spacetime inside black holes. Quantum superposition of microstate geometries. Not some hand-waving idea - provable by rigorous calculations in String Theory Mittwoch, 12. März 2014 Other formulations: e.g. Bena, Warner, 2007 - Thermodynamics (EF T) breaks down at horizon. New low-mass d.o.f. kick in. Highly Unusual - No spacetime inside black holes. Quantumin this field superposition of microstate geometries. ☺ Not some hand-waving idea - provable by rigorous calculations in String Theory Mittwoch, 12. März 2014 Word of caution • To replace classical BH by BH-sized object – Gravastar – Infinite density firewall hovering above horizon – LQG configuration – Quark-star, you name it … – satisfy 2 very stringent tests: Horowitz Mittwoch, 12. März 2014 Word of caution • To replace classical
Load more

Recommended publications
  • Exotic Compact Objects Interacting with Fundamental Fields Engineering
    Exotic compact objects interacting with fundamental fields Nuno André Moreira Santos Thesis to obtain the Master of Science Degree in Engineering Physics Supervisors: Prof. Dr. Carlos Alberto Ruivo Herdeiro Prof. Dr. Vítor Manuel dos Santos Cardoso Examination Committee Chairperson: Prof. Dr. José Pizarro de Sande e Lemos Supervisor: Prof. Dr. Carlos Alberto Ruivo Herdeiro Member of the Committee: Dr. Miguel Rodrigues Zilhão Nogueira October 2018 Resumo A astronomia de ondas gravitacionais apresenta-se como uma nova forma de testar os fundamentos da física − e, em particular, a gravidade. Os detetores de ondas gravitacionais por interferometria laser permitirão compreender melhor ou até esclarecer questões de longa data que continuam por responder, como seja a existência de buracos negros. Pese embora o número cumulativo de argumentos teóricos e evidências observacionais que tem vindo a fortalecer a hipótese da sua existência, não há ainda qualquer prova conclusiva. Os dados atualmente disponíveis não descartam a possibilidade de outros objetos exóticos, que não buracos negros, se formarem em resultado do colapso gravitacional de uma estrela suficientemente massiva. De facto, acredita-se que a assinatura do objeto exótico remanescente da coalescência de um sistema binário de objetos compactos pode estar encriptada na amplitude da onda gravitacional emitida durante a fase de oscilações amortecidas, o que tornaria possível a distinção entre buracos negros e outros objetos exóticos. Esta dissertação explora aspetos clássicos da fenomenologia de perturbações escalares e eletromagnéticas de duas famílias de objetos exóticos cuja geometria, apesar de semelhante à de um buraco negro de Kerr, é definida por uma superfície refletora, e não por um horizonte de eventos.
    [Show full text]
  • SNOWMASS21-TF1 TF0-057.Pdf 409.50KB 2020-08-31 21:46:42
    Snowmass2021 - Letter of Interest Peering inside Black Holes with Gravitational Waves Thematic Areas: (TF01) String theory, quantum gravity, black holes (TF2) Effective field theory techniques (TF3) CFT and formal QFT (TF4) Scattering amplitudes (TF5) Lattice gauge theory (TF6) Theory techniques for precision physics (TF7) Collider phenomenology (TF8) BSM model building (TF9) Astro-particle physics & cosmology (TF10) Quantum Information Science (TF11) Theory of neutrino physics (CF6) Dark Energy and Cosmic Acceleration: Complementarity of Probes and New Facilities (CF7) Cosmic Probes of Fundamental Physics Contact Information: Emil Mottola (Los Alamos National Laboratory & Perimeter Institute)[[email protected]] Author: Emil Mottola Abstract: In classical General Relativity (GR) the interiors of Black Holes (BHs) are not only singular but, if rotating, also admit closed timelike curves, violating causality.1 This feature occurs at macroscopic distance scales, far larger than the microscopic Planck scale LP l. When quantum effects are considered, severe conflicts with statistical thermodynamics, conservation of probability and an enormous BH entropy arise also at the macroscopic horizon scale.2,3 This suggests that a low energy semi-classical Effective Field Theory (EFT) approach should be applicable. In this LOI such an approach based the conformal anomaly is proposed, which leads to a non-singular horizonless, but ultra-compact object called a gravitational condensate star. The gravastar hypothesis can be tested by searching for discrete surface modes and GW echoes emitted after binary merger events. In this new era of GW and multi-messenger astronomy with additional GW detectors coming online in this decade, the time is now ripe for a full-fledged effort to confront these theoretical ideas with the observational data that hold the promise of resolving the conundrum that BHs pose, and potentially point to a new path to ultimate synthesis of gravitation and quantum theory.
    [Show full text]
  • Arxiv:2010.05354V1 [Gr-Qc] 11 Oct 2020
    Black hole or Gravastar? The GW190521 case I. Antoniou1, ∗ 1Department of Physics, University of Ioannina, GR-45110, Ioannina, Greece (Dated: August 31, 2021) The existence of cosmological compact objects with very strong gravity is a prediction of General Relativity and an exact solution of the Einstein equations. These objects are called black holes and recently we had the first observations of them. However, the theory of black hole formation has some disadvantages. In order to avoid these, some scientists suggest the existence of gravastars (gravitation vacuum stars), an alternative stellar model which seems to solve the problems of the black hole theory. In this work we compare black holes and gravastars using a wide range of the literature and we emphasize the properties of gravastars, which are consistent with the current cosmological observations. Also, we propose gravastars as the solution of the ”pair-instability” effect and a possible explanation for the observed masses of the compact objects, before the collapse, from the gravitational signal GW190521, since in the formation of a gravastar there aren’t mass restrictions. PACS numbers: 98.62.Ai, 04.20.Cv, 04.30.-w I. INTRODUCTION black holes, or some other compact object with very strong gravity. Many scientists dispute the One of the most attractive concepts in Gen- existence of black holes because if we take into ac- eral Relativity is the existence and the properties count quantum effects, the gravitational collapse of black holes, a region of spacetime where grav- of objects comes to a halt and furthermore no ity is so strong that nothing, no particles or even event horizon forms [2].
    [Show full text]
  • Arxiv:1607.03593V1 [Gr-Qc] 13 Jul 2016 Hc Ssilukona Ula N H Super-Nuclear the to and Core, Nuclear Used Densities
    Tidal deformability and I-Love-Q relations for gravastars with polytropic thin shells 1,2 3 † 4,5‡ Nami Uchikata ,∗ Shijun Yoshida , and Paolo Pani 1Department of Physics, Rikkyo University, Nishi-ikebukuro, Toshima-ku, Tokyo 171-8501, Japan 2Department of Mathematics and Physics, Graduate School of Science, Osaka City University, Sumiyoshi-ku, Osaka 558-8585, Japan 3Astronomical Institute, Tohoku University, Aramaki-Aoba, Aoba-ku, Sendai 980-8578, Japan 4Dipartimento di Fisica, ”Sapienza” Universit`adi Roma & Sezione INFN Roma1, Piazzale Aldo Moro 5, 00185 Roma, Italy 5Centro Multidisciplinar de Astrof´ısica — CENTRA, Departamento de F´ısica, Instituto Superior T´ecnico — IST, Universidade de Lisboa - UL, Av. Rovisco Pais 1, 1049-001 Lisboa, Portugal (Dated: July 14, 2016) The moment of inertia, the spin-induced quadrupole moment, and the tidal Love number of neutron-star and quark-star models are related through some relations which depend only mildly on the stellar equation of state. These “I-Love-Q” relations have important implications for astro- physics and gravitational-wave astronomy. An interesting problem is whether similar relations hold for other compact objects and how they approach the black-hole limit. To answer these questions, here we investigate the deformation properties of a large class of thin-shell gravastars, which are exotic compact objects that do not possess an event horizon nor a spacetime singularity. Working in a small-spin and small-tidal field expansion, we calculate the moment of inertia, the quadrupole moment, and the (quadrupolar electric) tidal Love number of gravastars with a polytropic thin shell. The I-Love-Q relations of a thin-shell gravastar are drastically different from those of an ordinary neu- tron star.
    [Show full text]
  • Isotropic Gravastar Model in Rastall Gravity
    Hindawi Advances in Astronomy Volume 2020, Article ID 8861168, 10 pages https://doi.org/10.1155/2020/8861168 Research Article Isotropic Gravastar Model in Rastall Gravity G. Abbas and K. Majeed Department of Mathematics, e Islamia University of Bahawalpur, Bahawalpur, Pakistan Correspondence should be addressed to G. Abbas; [email protected] Received 26 September 2020; Revised 28 October 2020; Accepted 4 November 2020; Published 16 November 2020 Academic Editor: Yu Liu Copyright © 2020 G. Abbas and K. Majeed. ,is is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. In the present paper, we have introduced a new model of gravastar with an isotropic matter distribution in Rastall gravity by the Mazur–Mottola (2004) mechanism. Mazur–Mottola approach is about the construction of gravastar which is predicted as an alternative to black hole. By following this convention, we define gravastar in the form of three phases. ,e first one is an interior phase which has negative density; the second part consists of thin shell comprising ultrarelativistic stiff fluid for which we have discussed the length, energy, and entropy. By the graphical analysis of entropy, we have shown that our proposed thin shell gravastar model is potentially stable. ,e third phase of gravastar is defined by the exterior Schwarzschild geometry. For the interior of gravastar, we have found the analytical solutions free from any singularity and the event horizon in the framework of Rastall gravity. 1. Introduction For the very first time, in the 18th century, Laplace and It was required to formulate such an alternative system Michell gave the clues of existence of a celestial body having that could tackle the abovementioned challenges; then, in extreme density and strongest gravitational effect enough 2001, Mazur and Mottola [10, 11] suggested a marvelous idea that even the light cannot be escaped.
    [Show full text]
  • The Unique Potential of Extreme Mass-Ratio Inspirals for Gravitational-Wave Astronomy 1, 2 3, 4 Christopher P
    Main Thematic Area: Formation and Evolution of Compact Objects Secondary Thematic Areas: Cosmology and Fundamental Physics, Galaxy Evolution Astro2020 Science White Paper: The unique potential of extreme mass-ratio inspirals for gravitational-wave astronomy 1, 2 3, 4 Christopher P. L. Berry, ∗ Scott A. Hughes, Carlos F. Sopuerta, Alvin J. K. Chua,5 Anna Heffernan,6 Kelly Holley-Bockelmann,7 Deyan P. Mihaylov,8 M. Coleman Miller,9 and Alberto Sesana10, 11 1CIERA, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA 2Department of Physics and MIT Kavli Institute, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 3Institut de Ciencies` de l’Espai (ICE, CSIC), Campus UAB, Carrer de Can Magrans s/n, 08193 Cerdanyola del Valles,` Spain 4Institut d’Estudis Espacials de Catalunya (IEEC), Edifici Nexus I, Carrer del Gran Capita` 2-4, despatx 201, 08034 Barcelona, Spain 5Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA 6School of Mathematics and Statistics, University College Dublin, Belfield, Dublin 4, Ireland 7Department of Physics and Astronomy, Vanderbilt University and Fisk University, Nashville, TN 37235, USA 8Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK 9Department of Astronomy and Joint Space-Science Institute, University of Maryland, College Park, MD 20742-2421, USA 10School of Physics & Astronomy and Institute for Gravitational Wave Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK 11Universita` di Milano Bicocca, Dipartimento di Fisica G. Occhialini, Piazza della Scienza 3, I-20126, Milano, Italy (Dated: March 7, 2019) The inspiral of a stellar-mass compact object into a massive ( 104–107M ) black hole ∼ produces an intricate gravitational-wave signal.
    [Show full text]
  • Table of Contents (Print)
    PHYSICAL REVIEW D PERIODICALS For editorial and subscription correspondence, Postmaster send address changes to: please see inside front cover (ISSN: 1550-7998) APS Subscription Services P.O. Box 41 Annapolis Junction, MD 20701 THIRD SERIES, VOLUME 102, NUMBER 2 CONTENTS D15 JULY 2020 The Table of Contents is a total listing of Parts A, B and C. Part A consists of articles 020001–023528, Part B articles 023529–024061, and Part C articles 024062–029902(E) PART A EDITORIALS Editorial: The Future of Physical Review D (1 pages) .............................................................................. 020001 Mirjam Cvetič RAPID COMMUNICATIONS Universal upper bound on the inflationary energy scale from the trans-Planckian censorship conjecture (7 pages) ...... 021301(R) Shuntaro Mizuno (水野俊太郎), Shinji Mukohyama (向山信治), Shi Pi (皮石), and Yun-Long Zhang (张云龙) Shift-symmetric orbital inflation: Single field or multifield? (6 pages) ........................................................... 021302(R) Ana Achúcarro, Edmund J. Copeland, Oksana Iarygina, Gonzalo A. Palma, Dong-Gang Wang, and Yvette Welling Constraint on the Yukawa suppression of the Newtonian potential from the planetary ephemeris INPOP19a (6 pages) 021501(R) L. Bernus, O. Minazzoli, A. Fienga, M. Gastineau, J. Laskar, P. Deram, and A. Di Ruscio Testing Brans-Dicke gravity with screening by scalar gravitational wave memory (6 pages) ................................ 021502(R) Kazuya Koyama Lightcone commutator and stress-tensor exchange in d>2 conformal field theories (6 pages) ............................. 021701(R) Kuo-Wei Huang ARTICLES Detection of cosmic structures using the bispectrum phase. I. Mathematical foundations (24 pages) ....................... 022001 Nithyanandan Thyagarajan and Chris L. Carilli Detection of cosmic structures using the bispectrum phase. II. First results from application to cosmic reionization using the Hydrogen Epoch of Reionization Array (19 pages) .................................................................
    [Show full text]
  • How to Tell a Gravastar from a Black Hole
    IOP PUBLISHING CLASSICAL AND QUANTUM GRAVITY Class. Quantum Grav. 24 (2007) 4191–4206 doi:10.1088/0264-9381/24/16/013 How to tell a gravastar from a black hole Cecilia B M H Chirenti1,2 and Luciano Rezzolla2,3 1 Instituto de F´ısica, Universidade de Sao˜ Paulo, Sao˜ Paulo, Brazil 2 Max-Planck-Institut fur¨ Gravitationsphysik, Albert Einstein Institut, 14476 Golm, Germany 3 Department of Physics, Louisiana State University, Baton Rouge, LA 70803, USA Received 11 June 2007, in final form 29 June 2007 Published 31 July 2007 Online at stacks.iop.org/CQG/24/4191 Abstract Gravastars have been recently proposed as potential alternatives to explain the astrophysical phenomenology traditionally associated with black holes, raising the question of whether the two objects can be distinguished at all. Leaving aside the debate about the processes that would lead to the formation of a gravastar and the astronomical evidence in their support, here we address two basic questions: is a gravastar stable against generic perturbations? If it is stable, can an observer distinguish it from a black hole of the same mass? To answer these questions we construct a general class of gravastars and determine the conditions they must satisfy in order to exist as equilibrium solutions of the Einstein equations. For such models we perform a systematic stability analysis against axial perturbations, computing the real and imaginary parts of the eigenfrequencies. Overall, we find that gravastars are stable to axial perturbations, but also that their quasi-normal modes differ from those of a black hole of the same mass and thus can be used to discern, beyond dispute, a gravastar from a black hole.
    [Show full text]
  • Astronomy February 18, 2013
    Outline of Astronomy February 18, 2013 Contents PHYS>Astronomy ............................................................................................................................................................. 1 PHYS>Astronomy>Universe ........................................................................................................................................ 2 PHYS>Astronomy>Universe>Cosmology .............................................................................................................. 5 PHYS>Astronomy>Universe>Cosmology>Energy .......................................................................................... 15 PHYS>Astronomy>Universe>Cosmology>Matter ........................................................................................... 16 PHYS>Astronomy>Universe>Cosmology>Matter>Particle ........................................................................ 17 PHYS>Astronomy>Universe>Cosmology>Radiation ...................................................................................... 17 PHYS>Astronomy>Universe>Cosmology>Singularity .................................................................................... 18 PHYS>Astronomy>Universe>Cosmology>Singularity>Black Hole ........................................................... 18 PHYS>Astronomy>Universe>Cosmology>Theories ........................................................................................ 22 PHYS>Astronomy>Universe>Cosmology>Theories>Inflation ..................................................................
    [Show full text]
  • The Digital Space Structure, Superconductor, and Superstar
    Global Journal of Science Frontier Research: A Physics and Space Science Volume 14 Issue 3 Version 1.0 Year 2014 Type : Double Blind Peer Reviewed International Research Journal Publisher: Global Journals Inc. (USA) Online ISSN: 2249-4626 & Print ISSN: 0975-5896 The Digital Space Structure, Superconductor, and Superstar By Ding-Yu Chung Abstract- In the digital space structure, space is digitalized by 1 and 0 for attachment space and detachment space, respectively. A special force field (the short-range extreme force field) can be derived from the digital space structure to generate superconductor at extremely low temperature and superstar at extremely high density. Singularity-free superstar is a model for the collapse of large stars and for GRBs, and as an alternative to black hole. Attachment space allows object to attach to account for rest mass and reversible movement, while detachment space allows no object to attach to account for irreversible kinetic energy. The combination of attachment space and detachment space brings about the three structures: binary partition space, miscible space, orbinary lattice space. Binary partition space (1)n(0)n consists of separated continuous phases of attachment space and detachment space to account for quantum mechanics and extreme force field. In miscible space (1+0)n, attachment space is miscible to detachment space without separation to account for special relativity. Keywords: space structure, quantum mechanics, force fields, superconductor, superstar, black hole, gravastar, GRB, collapsar, singularity. GJSFR-A Classification : FOR Code: 240203p TheDigitalSpaceStructureSuperconductorandSuperstar Strictly as per the compliance and regulations of : © 2014. Ding-Yu Chung. This is a research/review paper, distributed under the terms of the Creative Commons Attribution- Noncommercial 3.0 Unported License http://creativecommons.org/licenses/by-nc/3.0/), permitting all non commercial use, distribution, and reproduction in any medium, provided the original work is properly cited.
    [Show full text]
  • Approximate Universal Relations for Neutron Stars and Quark Stars
    Approximate universal relations for neutron stars and quark stars Authors: Kent Yagi and Nicolas Yunes NOTICE: this is the author’s version of a work that was accepted for publication in Physics Reports. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Physics Reports, VOL# 681, (March 2017). DOI# 10.1016/j.physrep.2017.03.002 Yagi, Kent , and Nicolas Yunes. "Approximate universal relations for neutron stars and quark stars." Physics Reports (March 2017). DOI: 10.1016/j.physrep.2017.03.002. Made available through Montana State University’s ScholarWorks scholarworks.montana.edu Approximate universal relations for neutron stars and quark stars Kent Yagi a,b,*, Nicolás Yunes b a Department of Physics, Princeton University, Princeton, NJ 08544, USA b eXtreme Gravity Institute, Department of Physics, Montana State University, Bozeman, MT 59717, USA Abstract Neutron stars and quark stars are ideal laboratories to study fundamental physics at supra nuclear densities and strong gravitational fields. Astrophysical observables, however, depend strongly on the star's internal structure, which is currently unknown due to uncertainties in the equation of state. Universal relations, however, exist among certain stellar observables that do not depend sensitively on the star's internal structure. One such set of relations is between the star's moment of inertia (I), its tidal Love number (Love) and its quadrupole moment (Q ), the so-called I–Love–Q relations.
    [Show full text]
  • Did GW150914 Produce a Rotating Gravastar?
    Did GW150914 produce a rotating gravastar? Cecilia Chirenti! CMCC - UFABC Work done in collaboration with ! Luciano Rezzolla (Frankfurt University) [arxiv:1602.08759v1] Black hole mimickers Possible models include:! gravastars! boson stars! wormholes! superspinars Gravastars [Mazur and Mottola, 2004] Alternative to the end state of stellar evolution! “gravitational vacuum condensate star”! almost as compact as a black hole! no event horizon or central singularity Formation of a gravastar Gravitational collapse of a massive star! Phase transition as stellar radius approaches its Schwarzschild radius…! … leading to the formation of a de Sitter core!! Baryonic mass of the stars becomes a shell of stiff matter surrounding the core! (Speculation!) Original gravastar model δ = r r 2 − 1 Interior! 0 r r , ⇢ = p µ = M/r2 1 − ! Shell! r r r , ⇢ =+p 1 2 ! Exterior! r r, ⇢ = p =0 2 5-layer model! Other gravastars 3-layer model (infinitesimally thin shell of matter) [Wisser and Wiltshire, 2004]! Fluid gravastar model (no shells) [Cattoen, Faber and Visser, 2005]! Electrically charged gravastars [Horvat, Ilijic and Marunovic, 2009]! Magnetized gravastars [Turimov,Ahmedov and Abdujabbarov, 2009]! Rotating gravastars [Uchikata and Yoshida, 2016]! etc… Stability of a gravastar Non-rotating gravastars:! Radial oscillations [Visser and Wiltshire, 2004; Horvat, Ilijic and Marunovic, 2011]! Gravitational (polar and axial) perturbations [DeBenedictis et al., 2006; Chirenti and Rezzolla, 2008; Pani et al., 2009]! Rotating gravastars:! Scalar perturbations
    [Show full text]