Jacob Bekenstein, Towering Theoretical Physicist Who Studied Black Holes, Dies at 68
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Stephen Hawking (1942–2018) World-Renowned Physicist Who Defied the Odds
COMMENT OBITUARY Stephen Hawking (1942–2018) World-renowned physicist who defied the odds. hen Stephen Hawking was speech synthesizer processed his words and diagnosed with motor-neuron generated the androidal accent that became disease at the age of 21, it wasn’t his trademark. In this way, he completed his Wclear that he would finish his PhD. Against best-selling book A Brief History of Time all expectations, he lived on for 55 years, (Bantam, 1988), which propelled him to becoming one of the world’s most celebrated celebrity status. IAN BERRY/MAGNUM scientists. Had Hawking achieved equal distinction Hawking, who died on 14 March 2018, was in any other branch of science besides cos- born in Oxford, UK, in 1942 to a medical- mology, it probably would not have had the researcher father and a philosophy-graduate same resonance with a worldwide public. As mother. After attending St Albans School I put it in The Telegraph newspaper in 2007, near London, he earned a first-class degree “the concept of an imprisoned mind roaming in physics from the University of Oxford. He the cosmos” grabbed people’s imagination. began his research career in 1962, enrolling In 1965, Stephen married Jane Wilde. as a graduate student in a group at the Uni- After 25 years of marriage, and three versity of Cambridge led by one of the fathers children, the strain of Stephen’s illness of modern cosmology, Dennis Sciama. and of sharing their home with a team of The general theory of relativity was at that nurses became too much and they sepa- time undergoing a renaissance, initiated in rated, divorcing in 1995. -
Black Holes and Qubits
Subnuclear Physics: Past, Present and Future Pontifical Academy of Sciences, Scripta Varia 119, Vatican City 2014 www.pas.va/content/dam/accademia/pdf/sv119/sv119-duff.pdf Black Holes and Qubits MICHAEL J. D UFF Blackett Labo ratory, Imperial C ollege London Abstract Quantum entanglement lies at the heart of quantum information theory, with applications to quantum computing, teleportation, cryptography and communication. In the apparently separate world of quantum gravity, the Hawking effect of radiating black holes has also occupied centre stage. Despite their apparent differences, it turns out that there is a correspondence between the two. Introduction Whenever two very different areas of theoretical physics are found to share the same mathematics, it frequently leads to new insights on both sides. Here we describe how knowledge of string theory and M-theory leads to new discoveries about Quantum Information Theory (QIT) and vice-versa (Duff 2007; Kallosh and Linde 2006; Levay 2006). Bekenstein-Hawking entropy Every object, such as a star, has a critical size determined by its mass, which is called the Schwarzschild radius. A black hole is any object smaller than this. Once something falls inside the Schwarzschild radius, it can never escape. This boundary in spacetime is called the event horizon. So the classical picture of a black hole is that of a compact object whose gravitational field is so strong that nothing, not even light, can escape. Yet in 1974 Stephen Hawking showed that quantum black holes are not entirely black but may radiate energy, due to quantum mechanical effects in curved spacetime. In that case, they must possess the thermodynamic quantity called entropy. -
Arxiv:1410.1486V2 [Gr-Qc] 26 Aug 2015
October 2014 Black Hole Thermodynamics S. Carlip∗ Department of Physics University of California Davis, CA 95616 USA Abstract The discovery in the early 1970s that black holes radiate as black bodies has radically affected our understanding of general relativity, and offered us some early hints about the nature of quantum gravity. In this chapter I will review the discovery of black hole thermodynamics and summarize the many indepen- dent ways of obtaining the thermodynamic and (perhaps) statistical mechanical properties of black holes. I will then describe some of the remaining puzzles, including the nature of the quantum microstates, the problem of universality, and the information loss paradox. arXiv:1410.1486v2 [gr-qc] 26 Aug 2015 ∗email: [email protected] 1 Introduction The surprising discovery that black holes behave as thermodynamic objects has radically affected our understanding of general relativity and its relationship to quantum field theory. In the early 1970s, Bekenstein [1, 2] and Hawking [3, 4] showed that black holes radiate as black bodies, with characteristic temperatures and entropies ~κ Ahor kTH = ;SBH = ; (1.1) 2π 4~G where κ is the surface gravity and Ahor is the area of the horizon. These quantities appear to be inherently quantum gravitational, in the sense that they depend on both Planck's constant ~ and Newton's constant G. The resulting black body radiation, Hawking radiation, has not yet been directly observed: the temperature of an astrophysical black hole is on the order of a microkelvin, far lower than the cosmic microwave background temperature. But the Hawking temperature and the Bekenstein-Hawking entropy have been derived in so many independent ways, in different settings and with different assumptions, that it seems extraordinarily unlikely that they are not real. -
Arxiv:1202.4545V2 [Physics.Hist-Ph] 23 Aug 2012
The Relativity of Existence Stuart B. Heinrich [email protected] October 31, 2018 Abstract Despite the success of modern physics in formulating mathematical theories that can predict the outcome of experiments, we have made remarkably little progress towards answering the most fundamental question of: why is there a universe at all, as opposed to nothingness? In this paper, it is shown that this seemingly mind-boggling question has a simple logical answer if we accept that existence in the universe is nothing more than mathematical existence relative to the axioms of our universe. This premise is not baseless; it is shown here that there are indeed several independent strong logical arguments for why we should believe that mathematical existence is the only kind of existence. Moreover, it is shown that, under this premise, the answers to many other puzzling questions about our universe come almost immediately. Among these questions are: why is the universe apparently fine-tuned to be able to support life? Why are the laws of physics so elegant? Why do we have three dimensions of space and one of time, with approximate locality and causality at macroscopic scales? How can the universe be non-local and non-causal at the quantum scale? How can the laws of quantum mechanics rely on true randomness? 1 Introduction can seem astonishing that anything exists” [73, p.24]. Most physicists and cosmologists are equally perplexed. Over the course of modern history, we have seen advances in Richard Dawkins has called it a “searching question that biology, chemistry, physics and cosmology that have painted rightly calls for an explanatory answer” [26, p.155], and Sam an ever-clearer picture of how we came to exist in this uni- Harris says that “any intellectually honest person will admit verse. -
Brief Newsletter from World Scientific February 2017
Brief Newsletter from World Scientific February 2017 Exclusive Interview with 2003 Nobel Laureate One of the Top Condensed Matter Theorists and World Scientific Author Anthony Leggett Sir Professor Anthony James Leggett is a distinguished physicist who was awarded the Nobel Prize in Physics in 2003 for his pioneering contributions to the theory of superconductors and superfluids. He is currently a professor at the University of Illinois at Urbana-Champaign. Prof Leggett gave a presentation at the 2016 APS March Meeting in Baltimore, USA on “Reflections on the past, present and future of condensed matter physics”. In a phone interview, he shared with us some of his thoughts and further musings on the future of condensed matter physics. Paradigm Shift and Our Quest for the Unknown Chad Hollingsworth Your talk at the APS March Meeting 2016 mentioned developments That probably depends on your current tenure status! Certainly, if that you classified as “paradigm shifts”. Are there any recent you have a secure, tenured job (as I have been fortunate enough to discoveries that you would classify as paradigm shifts? have for the last few decades), then I think most certainly it’s better Well, if we go slightly outside the area of condensed matter physics to explore the unknown. But, of course, I appreciate that in the current as it has been conventionally defined, then, undoubtedly, any employment situation, people who have not got a tenured job need revolution which overthrew the view of quantum mechanics as a to think about their future. This may well be a rather strong pressure complete account of the world would, I think, certainly qualify as a to basically explore the known further. -
Upper Limit on the Thermodynamic Information Content of an Action Potential
Preprints (www.preprints.org) | NOT PEER-REVIEWED | Posted: 4 February 2020 Upper limit on the thermodynamic information content of an action potential Sterling Street∗ Department of Cellular Biology, Franklin College of Arts and Sciences, University of Georgia, Athens, GA, USA February 2, 2020 Abstract In computational neuroscience, spiking neurons are often analyzed as computing devices that register bits of information, with each ac- tion potential carrying at most one bit of Shannon entropy. Here, I question this interpretation by using Landauer's principle to estimate an upper limit for the quantity of thermodynamic information that can be dissipated by a single action potential in a typical mammalian neuron. I show that an action potential in a typical mammalian cor- tical pyramidal cell can carry up to approximately 3.4 · 1011 natural units of thermodynamic information, or about 4.9 · 1011 bits of Shan- non entropy. This result suggests that an action potential can process much more information than a single bit of Shannon entropy. 1 Introduction \The fundamental constraint on brain design emerges from a law of physics. This law governs the costs of capturing, sending, and storing information. This law, embodied in a family of equa- tions developed by Claude Shannon, applies equally to a telephone line and a neural cable, equally to a silicon circuit and a neural circuit." { Peter Sterling and Simon Laughlin [1] ∗[email protected]. Keywords: information, entropy, energy, thermodynamics, Landauer's principle, action potential 1 © 2020 by the author(s). Distributed under a Creative Commons CC BY license. Preprints (www.preprints.org) | NOT PEER-REVIEWED | Posted: 4 February 2020 Many hypotheses and theories analyze spiking neurons as binary electro- chemical switches [1-3]. -
Edward Witten (Slides)
Introduction to Black Hole Thermodynamics Edward Witten, IAS Madan Lal Mehta Lecture, April 19, 2021 In the first half of this talk, I will explain some key points of black hole thermodynamics as it was developed in the 1970's. In the second half, I will explain some more contemporary results, though I will not be able to bring the story really up to date. I cannot explain all the high points in either half of the talk, unfortunately, as time will not allow. Black hole thermodynamics started with the work of Jacob Bekenstein (1972) who, inspired by questions from his advisor John Wheeler, asked what the Second Law of Thermodynamics means in the presence of a black hole. The Second Law says that, for an ordinary system, the \entropy" can only increase. However, if we toss a cup of tea into a black hole, the entropy seems to disappear. Bekenstein wanted to \generalize" the concept of entropy so that the Second Law would hold even in the presence of a black hole. For this, he wanted to assign an entropy to the black hole. What property of a black hole can only increase? It is not true that the black hole mass always increases. A rotating black hole, for instance, can lose mass as its rotation slows down. But there is a quantity that always increases: Stephen Hawking had just proved the \area theorem," which says that the area of the horizon of a black hole can only increase. So it was fairly natural for Bekenstein to propose that the entropy of a black hole should be a multiple of the horizon area. -
Arxiv:Quant-Ph/0101077 V1 17 Jan 2001 His Get When Rect W Y B Mals.” Cup of Ab of Miliar
100 Years of the Quantum Max Tegmark Dept. of Physics, Univ. of Pennsylvania, Philadelphia, PA 19104; [email protected] John Archibald Wheeler Princeton University, Department of Physics, Princeton, NJ 08544; [email protected] (An abbreviated version of this article, with much better graphics, was published in the Feb. 2001 issue of Scientific American, p.68-75.) Abstract: As quantum theory celebrates its 100th birthday, spectacular successes are mixed with outstanding puzzles and promises of new technologies. This article reviews both the successes of quantum theory and the ongoing debate about its consequences for issues ranging from quantum computation to consciousness, parallel universes and the nature of physical reality. We argue that modern experiments and the discovery of decoherence have have shifted prevailing quantum inter- pretations away from wave function collapse towards unitary physics, and discuss quantum processes in the framework of a tripartite subject-object-environment decomposition. We conclude with some speculations on the bigger picture and the search for a unified theory of quantum gravity. \...in a few years, all the great physical constants will ever, this involved an assumption so bizarre that even have been approximately estimated, and [...] the only oc- he distanced himself from it for many years afterwards: cupation which will then be left to the men of science will that energy was only emitted in certain finite chunks, or be to carry these measurement to another place of deci- \quanta". Yet this strange assumption proved extremely mals." As we enter the 21st century amid much brouhaha successful. Inspired by Planck's quantum hypothesis, Pe- about past achievements, this sentiment may sound fa- ter Debye showed that the strange thermal behavior of miliar. -
Unitarity Entropy Bound: Solitons and Instantons
Unitarity Entropy Bound: Solitons and Instantons Gia Dvali Arnold Sommerfeld Center, Ludwig-Maximilians-Universit¨at, Theresienstraße 37, 80333 M¨unchen, Germany, Max-Planck-Institut f¨ur Physik, F¨ohringer Ring 6, 80805 M¨unchen, Germany and Center for Cosmology and Particle Physics, Department of Physics, New York University, 726 Broadway, New York, NY 10003, USA (Dated: July 18, 2019) We show that non-perturbative entities such as solitons and instantons saturate bounds on entropy when the theory saturates unitarity. Simultaneously, the entropy becomes equal to the area of the soliton/instanton. This is strikingly similar to black hole entropy despite absence of gravity. We explain why this similarity is not an accident. We present a formulation that allows to apply the entropy bound to instantons. The new formulation also eliminates apparent violations of the Bekenstein entropy bound by some otherwise-consistent unitary systems. We observe that in QCD, an isolated instanton of fixed size and position violates the entropy bound for strong ’t Hooft coupling. At critical ’t Hooft coupling the instanton entropy is equal to its area. I. UNITARITY AND ENTROPY The explanation given in [4] to the above phenomenon is that the key role both in saturation of the entropy The Bekenstein entropy bound [1] (see also, [2]) bound as well as in its area-form is played by an inter- particle coupling constant α that controls perturbative Smax = MR, (1) unitarity of the theory. The idea is that the objects that puts an upper limit on the amount of information stored share the property (3) are maximally packed in the sense in a system of energy M and size R. -
Guide to Wolfgang Kurt Hermann Panofsky Papers, 1932-2008 Collection SLAC003 SLAC National Accelerator Laboratory, Stanford University
Guide to Wolfgang Kurt Hermann Panofsky Papers, 1932-2008 Collection SLAC003 SLAC National Accelerator Laboratory, Stanford University Contact Information: Archives, History & Records Office SLAC National Accelerator Laboratory 2575 Sand Hill Road MS97 Menlo Park, CA 94025 Phone: (650) 926-5376 Email: [email protected] URL: http://www.slac.stanford.edu/history/ ©2018 SLAC National Accelerator Laboratory. All rights reserved. Panofsky Papers Guide Contents Descriptive Summary...................................................................................................................... 2 Administrative Information ............................................................................................................ 2 Biographical Note ....................................................................................................................... 3 Scope and Content .................................................................................................................... 12 Arrangement ............................................................................................................................. 12 Related Material ........................................................................................................................ 21 1 Panofsky Papers Guide Descriptive Summary Title: Wolfgang Kurt Hermann Panofsky Papers, 1932-2008 Collection Number: SLAC003 Creator: Panofsky, Wolfgang Kurt Hermann Extent: 220 cubic feet Repository: Stanford University. SLAC National Accelerator Laboratory. -
Quantum Gravity: a Primer for Philosophers∗
Quantum Gravity: A Primer for Philosophers∗ Dean Rickles ‘Quantum Gravity’ does not denote any existing theory: the field of quantum gravity is very much a ‘work in progress’. As you will see in this chapter, there are multiple lines of attack each with the same core goal: to find a theory that unifies, in some sense, general relativity (Einstein’s classical field theory of gravitation) and quantum field theory (the theoretical framework through which we understand the behaviour of particles in non-gravitational fields). Quantum field theory and general relativity seem to be like oil and water, they don’t like to mix—it is fair to say that combining them to produce a theory of quantum gravity constitutes the greatest unresolved puzzle in physics. Our goal in this chapter is to give the reader an impression of what the problem of quantum gravity is; why it is an important problem; the ways that have been suggested to resolve it; and what philosophical issues these approaches, and the problem itself, generate. This review is extremely selective, as it has to be to remain a manageable size: generally, rather than going into great detail in some area, we highlight the key features and the options, in the hope that readers may take up the problem for themselves—however, some of the basic formalism will be introduced so that the reader is able to enter the physics and (what little there is of) the philosophy of physics literature prepared.1 I have also supplied references for those cases where I have omitted some important facts. -
The Bekenstein Bound and Non-Perturbative Quantum Gravity
enstein b ound and View metadata, citation and similar papers at core.ac.uk The Bek brought to you by CORE provided by CERN Document Server non-p erturbative quantum gravity Kirill V.Krasnov Bogolyubov Institute for Theoretical Physics, Kiev 143, Ukraine (March 19, 1996) We study quantum gravitational degrees of freedom of an arbitrarily chosen spatial region in the framework of lo op quantum gravity . The main question concerned is if the dimension of the Hilb ert space of states corresp onding to the same b oundary area satis es the Bekenstein b ound. We show that the dimension of such space formed by all kinematical quantum states, i.e. with the Hamiltonian constraint b eing not imp osed, is in nite. We make an assumption ab out the Hamiltonian's action, which is equivalent to the holographic hyp othesis, an which lead us to physical states (solutions of the Hamiltonian constraint) sp eci ed by data on the b oundary. The physical states which corresp ond to the same b oundary area A form a nite dimensional Hilb ert space and we show that its dimension 2 , where lies in the interval 0:55 < < 1:01. We discuss in general the is equial to exp A=l p arising notion of statistical mechanical entropy.For our particular case, when the only parameter sp ecifying the system's macrostate is the b oundary area, this entropy is given by S (A)= A.We discuss the p ossible implications of the result obtained for the black hole entropy. Among the results of the lo op approach to non-p erturbative quantum gravity the are several which, if taken seriously, tell us that the picture of geometry on scales small comparatively with our usual scales (on Planckian scales) lo oks quite di erently from the habitual picture of Riemannian geometry, and that the usual classical picture arises only on a coarse-graining.