In this note we have applied directly the Shannon formula for information theory entropy to derive the Black Hole (Bekenstein-Hawking) entropy. But if black holes had entropy, they would have to emit radiation (which was thought impossible at the time). The basic physical reasoning is that the area of its horizon is the only physical geometry-related quantity that a black hole can actually have. After a brief review of the elements of the theory of information, we discuss black . with f ( r) = k 2 ( r 2 − μ 2) and μ 2 = 8 G n M k 2 . An important black hole observable is the Bekenstein-Hawking (BH) entropy, which is proportional to the area of the event horizon, SBH = Ah / (4 G ). Quantum information is entangled, all the information accumulated inside the black hole is conserved after the evaporation of the black hole. Most striking is the similarity in the behaviors of black-hole area and of entropy: Both quantities tend to increase irreversibly. . The black hole entropy can be obtained through number of ways. However, by obtaining a precise first law of black hole mechanics, it was clear that if one wishes to assign a physical entropy to a black hole proportional to its area, A, then one must also must also assign to it a This is particularly true for the first and second laws. . ( 7)and(8)showthatsuchacorrespondence is consistent only if the black hole entropy has the Bekenstein-Hawking value, and endow . Bekenstein (1974) J. D. Bekenstein, Phys. ~) By common entropy we mean entropy in the black-hole's exterior. Table of Content; Relativity Science Calculator There are a number of similarities between black-hole physics and thermodynamics. The generalised second law inspired Bekenstein to a little thought experiment which gave rise to the Bekenstein bound on information. Hot deals; Introduction. Indeed, through Bekenstein bound, [4], one can see that the black hole entropy, as described by the area law, is the maximal entropy that can be achieved and this was the main hint that led to the holographic principle, [5]. Proposal : Geometric Entropy • in a theory of quantum gravity, for any sufficiently large region Categories. The increase in the black hole entropy will compensate, and most frequently over-compensate, for the loss in the ordinary entropy outside it. In ( perturbative) string theory the Bekenstein-Hawking entropy associated to a macroscopic black hole finds an explanation as follows: The black hole spacetime is regarded as a strongly coupled condensate of string states ( closed strings, carrying gravity ). 10.8) where Planck's length is the denominator to Wheeler, who spoke of using Planck's length in conversation with Bekenstein on April 2, 1971. It ranks as one of the most important physics papers of the 20th century. This result is strong evidence that there is a gravity dual of the SY state with a AdS. The idea that black holes should have an entropy value associated with them was first championed by Jacob Bekenstein.It had been noticed by Stephen Hawking and others that the law 'the event horizon area of a black hole must always increase' is very similar to the second law of thermodynamics; 'the entropy of a closed system … The Bekenstein-Hawking entropy or black hole entropy is the amount of entropy that must be assigned to a black hole in order for it to comply with the laws of thermodynamics as they are interpreted by observers external to that black hole. • quantum gravity provides a fundamental scale. "Black holes and entropy". Most striking is the similarity in the behaviors of black-hole area and of entropy: Both quantities tend to increase irreversibly. BEKENSTEIN We state the second law as follows: r, Common entropy plus black-hole entropy never decreases. Hawking proved that during the combination process of two Kerr black holes into one Kerr black hole, the horizon area never decreases [9]. 738 J.D. Most striking is the similarity in the behaviors of black-hole area and of entropy: Both quantities tend to increase irreversibly. DOI: 10.1007/Bf02762768 : 1: 1973: Bekenstein JD. This was not for a four dimensional black hole, but a rotating five dimensional black hole in Kaluza-Klein theory. black hole formula by ramanujan. In this paper we make this similarity the basis of a thermodynamic approach to black-hole physics. By Jennifer Ouellette on August 17, 2015. In a follow-up four-page report published in 1972, Black Holes and the Second Law, Bekenstein reformulated this law: "Common entropy plus black-hole entropy never decreases" [4, p.738]. Credit: Public domain, via Wikimedia Commons. The scaling of Bekenstein entropy as the horizon area, S ∼ L 2 / L P 2, creates the impression that the horizon is a union of N Planck-size pixels each housing a distinguishable degree of freedom that . . Download and reference "Black Holes And Entropy" by J. Bekenstein on Citationsy I share some memories and offer a personal perspective on Jacob Bekenstein's legacy, focussing on black hole entropy and the Bekenstein bound. Quantum information is entangled, all the information accumulated inside the black hole is conserved after the evaporation of the black hole. A solar-mass black hole has SBH ∼ 1077k. Download: . Black-hole physics seems to provide at least two ways in which the second law of thermodynamics may be transcended or violated: a) Let an observer drop or lower a package of entropy into a black hole; the entropy of the exterior world decreases. As an explicit example, we study near extremal Banados-Teitelboim-Zanelli black holes and derive this claim from AdS{sub 3}/CFT{sub 2}. The second model can simply derive out the formula of black hole entropy in General Relativity. Answer (1 of 5): Entropy is a measure of the energy unavailable to do work. A pure state will have zero entropy, while a mixed state will have maximal von Neumann entropy. 2 Since the area Ais never decreasing during the black hole combination process, Ais proportional to the entropy S. Bekenstein considered . The metric of the BTZ black hole is. We find an upper bound on the mass of a black hole/white hole pair. The proportionality between black hole entropy and area is derived from classical thermodynamics. Wow. capital city club black members; how to play background music on twitch xbox one; connect 4 solver algorithm. According to Bekenstein, one can define black-hole entropy as follows: I summarize a number of fascinating recent developments that grew out of Bekenstein's pioneering contributions, from the Ryu-Takayanagi proposal to the Quantum Null Energy Condition. Current Price Index; Current Price Sheet Hawking-Bekenstein entropy. • extends to de Sitter horizons and Rindler horizons • window into quantum gravity?!? In this paper we make this similarity the basis of a thermodynamic approach to black-hole physics. - TBH = - 1 87rcgH' (1.4 SBH = CA, (l-5) 1 S=,, were first derived quantum mechanically. • extends to de Sitter horizons and Rindler horizons • window into quantum gravity?!? Ever since the pioneer works of Bekenstein and Hawking, black hole entropy has been known to have a quantum origin. Submission history Black Hole Entropy: • Bekenstein and Hawking: event horizons have entropy! edna livestock auction. The black-hole entropy is proportional to the area of its event horizon . If a system exists that violates the bound, i.e., by having too much entropy, Bekenstein argued that it would be possible to violate the second law of thermodynamics by lowering it into a black hole. This is accurate. Black holes and entropy J. Bekenstein Published 15 April 1973 Physics Physical Review D There are a number of similarities between black-hole physics and thermodynamics. . 11: 467-470. The Bekenstein-Hawking entropy formula for a black hole. For instance, Wald [6] has . Bekenstein, Jacob D. There are a number of similarities between black-hole physics and thermodynamics. depends only on the total horizon area--also a . And the black hole entropy is S b h = A h 4 G . It can be readily demonstrated that Bekenstein-Hawking black hole entropy is non-extensive, while the Hawking and the Unruh temperatures are non-intensive. 06.07.22 | Comment? As a result, the associated equations violate the laws of thermodynamics and can hold no place in the physical sciences. Most striking is the similarity in the behaviors of black-hole area and of entropy: Both quantities tend to increase irreversibly. The black hole entropy can be obtained through number of ways. Sad news reached Jen-Luc Piquant this morning via . The quantum mass spectrum of the Kerr black hole Lettere Al Nuovo Cimento Series 2. Furthermore, from an exterior observer's point of view a black hole in equilibrium has only three . Origins Bekenstein derived the bound from heuristic arguments involving black holes. Most striking is the similarity in the behaviors of black-hole area and of entropy: Both quantities tend to increase irreversibly. This is much greater than the entropy of the matter that collapsed to form it: Thermal radiation has the highest entropy of ordinary matter, but a ball of thermal . The temperature is inversely proportional to the mass: K, where g, the Planck mass. Bob Walance said: Jacob Bekenstein asserts that the entropy of a black hole is proportional to its area rather than its volume. For instance, Wald [6] has . We track the evolution of entropy and black holes in a cyclic universe that undergoes repeated intervals of expansion followed by slow contraction and a smooth (non-singular) bounce. There are a number of similarities between black-hole physics and thermodynamics. conjectures in modern physics. English: The Bekenstein-Hawking entropy of a black hole is proportional to the surface area of the black hole as expressed in Planck units. The scaling of Bekenstein entropy as the horizon area, S ∼ L 2 / L P 2, creates the impression that the horizon is a union of N Planck-size pixels each housing a distinguishable degree of freedom that . There are a number of similarities between black-hole physics and thermodynamics. Two models get the same result that the . In this paper we make this similarity the basis of a thermodynamic approach to black-hole physics. So, if an object falls into a black hole, it has effectiv. One looks for a corresponding weakly-coupled background for . The Mexican-born Israeli-American theoretical physicist J. Bekenstein was the first one to suggest that black holes, a region of spacetime where gravity is so strong that not even light can escape from it, should have a well-defined entropy. 16), 137, "An Alternative Approach to Black Hole Entropy." Bekenstein attributes the formulation of the equation (136, eq. 2. horizon. 752. In this paper we make this similarity the basis of a thermodynamic approach to black-hole physics. We point out that the entropy of (near) extremal black holes can be interpreted as the entanglement entropy of dual conformal quantum mechanics via AdS{sub 2}/CFT{sub 1}. In this kind of cyclic scenario, there is no big crunch and no chaotic mixmaster behavior. Most striking is the similarity in the behaviors of black-hole area and of entropy: Both quantities tend to increase irreversibly. Black holes and entropy Physical Review D. 7: 2333-2346. Jacob Bekenstein suggested that the area of a black hole was itself a measurement of its entropy. 1The von Neumann or entanglement entropy is a measure to quantify the entanglement and is given by: S = − Tr ρ log ρ. 2 RINDLER SPACE 22 Figure 2: The von Neumann entropy versus time for an evaporating black hole according to Hawking and Page 3 For the Earth's mass, K, while for a solar mass, nK, both less than the temperature of the cosmic microwave . Con-versely, assuming the existence of a gravity dual, Eqs. (8) for the Bekenstein-Hawking entropy of AdS. Home; Our Products; About Us; Our Team; Contact; Order Now. In this paper we make this similarity the basis of a thermodynamic approach to black-hole physics. Quantum entropy of a black hole is a quantum generalization of the celebrated Bekenstein-Hawking area formula. The relationship between the classical and quantum . Every object has some amount of entropy. Its volume doesn't work because there's . Another black hole mystery is the origin of Bekenstein entropy and the quantum mechanism of information storage and processing by a black hole. Rev. Hot deals. Jacob Bekenstein, a physicist who prevailed in an argument with Stephen Hawking that revolutionized the study of black holes, and indeed the nature of space-time itself, died on Sunday in Helsinki . After recalling the definition of black holes, and reviewing their energetics and their classical thermodynamics, one expounds the conjecture of Bekenstein, attributing an entropy to black holes, and the calculation by Hawking of the semi-classical radiation spectrum of a black hole, involving a thermal (Planckian) factor. But this quite unusual for an entropy. Extraction of energy and charge from a black hole Physical Review D. 7: 949-953. It is important to point out that, as the stationary Kerr-Newman black hole is a non-static isolated horizon, further insights on the issues here discussed are necessary for a complete understanding of the nature of the black hole entropy calculation including rotating horizons. Recently a precise calculation of the entropy of a neutral black hole in string theory was achieved (Emparan and GH, 2006). For the 3-brane solution (3.1), the horizon is located at r = r0. II. Physical Review D 7(8): 2333-2346. has been cited by the following article: . conjectures in modern physics. The Bekenstein-Hawking entropy is a statement about the gravitational entropy of a system. Bekenstein bound is entropy of a black hole. According to the Bekenstein-Hawking theory, the temperature of a black hole is given by and the emitted radiation follows a blackbody distribution. Physicist Werner Israel also positioned himself against Bekenstein's views. Download Citation | Black hole entropy and the Bekenstein bound | I share some memories and offer a personal perspective on Jacob Bekenstein's legacy, focussing on black hole entropy and the . reproduce the entropy of all black holes, but this argument does not reproduce the entropy exactly. S = A/4ℓ_p^2 for ℓ = √ {Għ/c^3} and A = 4πr_s^2 and r_s . Bekenstein's 1972 proposal that black holes carry entropy Bek72 takes up four very small pages in a now extinct journal. BEKENSTEIN-HAWKING BLACK HOLE ENTROPY The Bekenstein-Hawking black hole entropy equation is A hG c k S B 2 π 3 = , (1) where S is entropy, c is the speed of light in vacuum, kB is Boltzmann's constant, h is Planck's constant, G is the universal constant of gravitation, and A is the area of the Yup. Furthermore, it has long been argued by Bekenstein that entropy should be quantized in discrete (equidistant) steps given its. Download Citation | Black hole entropy and the Bekenstein bound | I share some memories and offer a personal perspective on Jacob Bekenstein's legacy, focussing on black hole entropy and the . 2. horizons. The fact that black holes obey such laws was, in some sense, supportive of Bekenstein's thermodynamic ideas. Black Holes (BH) are, quite paradoxically, the simplest objects to describe (thermodynamically) in terms of Bekenstein-Hawking entropy, Hawking temperature etc. Bekenstein bound is entropy of a black hole. • quantum gravity provides a fundamental scale. Indeed, through Bekenstein bound, [4], one can see that the black hole entropy, as described by the area law, is the maximal entropy that can be achieved and this was the main hint that led to the holographic principle, [5]. After a brief review of the elements of the theory of information, we discuss black . The Bekenstein-Hawking entropy is a statement about the gravitational entropy of a system. After a brief review of the elements of the theory of information, we discuss black . DOI: 10.1103/Physrevd.7.949 : 1: 1973: Bekenstein JD. systems with a black hole to determine the entropy normalization.