Journal articles: 'Black hole physics'

1

Zakharov, Aleksandr F. "Black hole physics." Physics-Uspekhi 42, no. 9 (September 30, 1999): 947–51. http://dx.doi.org/10.1070/pu1999v042n09abeh000651.

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Zakharov, A. F. "Black hole physics." Uspekhi Fizicheskih Nauk 169, no. 9 (1999): 1041. http://dx.doi.org/10.3367/ufnr.0169.199909h.1041.

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Voss, D. "PHYSICS: Black Hole Encryption." Science 311, no. 5767 (March 17, 2006): 1525a. http://dx.doi.org/10.1126/science.311.5767.1525a.

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VISSER, MATT. "HAWKING RADIATION: A PARTICLE PHYSICS PERSPECTIVE." Modern Physics Letters A 08, no. 18 (June 14, 1993): 1661–70. http://dx.doi.org/10.1142/s0217732393001409.

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It has recently become fashionable to regard black holes as elementary particles. By taking this suggestion reasonably seriously it is possible to cobble together an elementary particle physics based on estimate for the decay rate (black hole) i → (black hole) f+ (massless quantum) . This estimate of the spontaneous emission rate contains two free parameters which may be fixed by demanding that the high energy end of the spectrum of emitted quanta match a black body spectrum at the Hawking temperature. The calculation, though technically trivial, has important conceptual implications: (1) The existence of Hawking radiation from black holes seems ultimately dependent only on the fact that massless quanta (and all other forms of matter) couple to gravity. (2) The essentially thermal nature of the Hawking spectrum seems to depend only on the fact that the number of internal states of a large mass black hole is enormous. (3) Remarkably, the resulting formula for the decay rate gives meaningful answers even when extrapolated to low mass black holes. The analysis seems to support the scenario of complete evaporation as the end point of the Hawking radiation process (no naked singularity, no stable massive remnant).

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Abramovsky. "Abramovsky—Gribov—Kancheli Theorem in the Physics of Black Holes." Physics 1, no. 2 (August 1, 2019): 253–70. http://dx.doi.org/10.3390/physics1020020.

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The proof of the Abramovsky—Gribov—Kancheli (AGK) theorem for black hole physics is given. Based on the AGK relations, a formula for the luminosity of a black hole as a function of the mass of the black hole is derived. The correspondence to experimental data is considered. It is shown that the black holes of the galaxies NGC3842 and NGC4889 do not differ from those of the other galaxies.

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Sims, Christopher. "Analogous Black Holes in Type-III Dirac Semimetal Ni3In2X2 (X = S, Se)." Crystals 13, no. 5 (May 20, 2023): 847. http://dx.doi.org/10.3390/cryst13050847.

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Black holes are objects that have a large mass and curve space time, characterized by their event horizon and singularity. Recently, an interesting concept of analogous black holes has emerged in the field of condensed matter physics. In this work, the possibility of realizing analogous black holes in topological material is Ni3In2X2 (X = S, Se) discussed. This work shows that the type-III Dirac cones of the material can lead to the emergence of an event horizon and the formation of a black hole-like region near the Dirac point. In addition, the possible experimental signatures of such a system are discussed and the potential implications of an analogous black hole for the study of black hole physics in condensed matter systems.

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Altas, E., and B. Tekin. "Basics of Apparent horizons in black hole physics." Journal of Physics: Conference Series 2191, no. 1 (February 1, 2022): 012002. http://dx.doi.org/10.1088/1742-6596/2191/1/012002.

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Abstract 1Event Horizon, a null hypersurface defining the boundary of the black hole region of a spacetime, is not particularly useful for evolving black holes since it is non-local in time. Instead, one uses the more tangible concept of Apparent Horizon for dynamical black holes out there in the sky that do all sorts of things: evolve, merge and feed on the environment. Event Horizon, being a gauge-independent, global property of the total spacetime is easy to define and locate in the stationary case; on the other hand, Apparent Horizon depends on the embedding of the surface in spacetime and hence it is somewhat tricky to define. But for numerical simulations in General Relativity, locating the Apparent Horizon helps one to excise the black hole region and the singularity to have a stable computation. Moreover, for stationary solutions cross-sections of these horizons match. Here we give a detailed pedagogical exposition of the subject and work out the non-trivial case of a slowly moving and spinning black hole.

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Poudel, Parashu Ram. "The Black Hole." Himalayan Physics 3 (December 26, 2012): 50–55. http://dx.doi.org/10.3126/hj.v3i0.7277.

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Black holes are the cold remnants of former stars. They are so dense that no matter -not even light - is able to escape their powerful gravitational pull. These are interesting objects from a fundamental physics point of view and play an important role in astrophysics. The knowledge of phenomenon of origin of black hole may lead to new understanding of the nature of the real universe. The Himalayan PhysicsVol. 3, No. 32012Page : 50-55

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Kubizňák, David, and Robert B. Mann. "Black hole chemistry." Canadian Journal of Physics 93, no. 9 (September 2015): 999–1002. http://dx.doi.org/10.1139/cjp-2014-0465.

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The mass of a black hole has traditionally been identified with its energy. We describe a new perspective on black hole thermodynamics, one that identifies the mass of a black hole with chemical enthalpy, and the cosmological constant as thermodynamic pressure. This leads to an understanding of black holes from the viewpoint of chemistry, in terms of concepts such as Van der Waals fluids, reentrant phase transitions, and triple points. Both charged and rotating black holes exhibit novel chemical-type phase behaviour, hitherto unseen.

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Frolov, Valery P. "Two-dimensional black hole physics." Physical Review D 46, no. 12 (December 15, 1992): 5383–94. http://dx.doi.org/10.1103/physrevd.46.5383.

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11

Tanaka, Takahiro. "Introduction to Black Hole Physics." Classical and Quantum Gravity 29, no. 14 (June 25, 2012): 149001. http://dx.doi.org/10.1088/0264-9381/29/14/149001.

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Nasution, Budiman, Winsyahputra Ritonga, Ruben Cornelius Siagian, Lulut Alfaris, Aldi Cahya Muhammad, Ukta Indra Nyuswantoro, and Gendewa Tunas Rancak. "Physics Visualization of Schwarzschild Black Hole through Graphic Representation of the Regge-Wheeler Equation using R-Studio Approach." Sainmatika: Jurnal Ilmiah Matematika dan Ilmu Pengetahuan Alam 20, no. 1 (June 30, 2023): 8–24. http://dx.doi.org/10.31851/sainmatika.v20i1.11845.

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This study aims to visualize the vibrations of black holes using the Regge-Wheeler equation in Cartesian coordinates. Black holes are astrophysical objects with extremely strong gravity, and understanding the vibrations around them provides insights into the nature and structure of black holes. The Regge-Wheeler equation is used to model these vibrations. In this study, the goal is to generate visual images that visualize the vibrations of black holes, including their frequencies, amplitudes, and possible vibration modes. Complex mathematical and computational methods were employed to create these visualizations. The findings of this research result in an intuitive and accurate visualizations of black hole vibrations. By observing the patterns and distributions of vibrations in visual form, complex concepts can be more easily understood and interpreted. These visualizations provide a better understanding of the characteristics of black hole vibrations and can serve as learning and comprehension tools for scientists and researchers. The accomplishment of this research addresses a deficiency in prior studies that lacked informative and intuitive visualizations of black hole vibration phenomena. The visualizations produced in this study make a significant contribution to our understanding of black hole vibration phenomena. The enhanced visualizations allow researchers to perceive patterns and distributions of vibrations more clearly, paving the way for new insights into the nature of black holes. The implications of this research are an improved understanding of black hole vibrations and a broader dissemination of knowledge about this phenomenon to the general public. The generated images can help communicate complex concepts more effectively, enhancing awareness and interest in black hole research.

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Aste, Andreas, and Dirk Trautmann. "Radial fall of a test particle onto an evaporating black hole." Canadian Journal of Physics 83, no. 10 (October 1, 2005): 1001–6. http://dx.doi.org/10.1139/p05-058.

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A test particle falling onto a classical black hole crosses the event horizon and ends up in the singularity within finite eigentime. In the "more realistic" case of a "classical" evaporating black hole, an observer falling onto a black hole observes a sudden evaporation of the hole. This illustrates the fact that the discussion of the classical process, commonly found in the literature, may become obsolete when the black hole has a finite lifetime. The situation is basically the same for more complex cases, for example, where a particle collides with two merging black holes. It should be pointed out that the model used in this paper is mainly of academic interest, since the description of the physics near a black-hole horizon still presents a difficult problem that is not yet fully understood, but our model provides a valuable possibility for students to enter the interesting field of black-hole physics and to perform numerical calculations of their own that are not very involved from the computational point of view.PACS Nos.: 04.25.g, 04.70.s, 04.70.Dy

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Liebling, Steven L. "Black hole critical phenomena without black holes." Pramana 55, no. 4 (October 2000): 497–509. http://dx.doi.org/10.1007/s12043-000-0162-6.

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Rizwan, Muhammad, and K. Saifullah. "GUP-corrected thermodynamics of accelerating and rotating black holes." International Journal of Modern Physics D 26, no. 05 (April 2017): 1741018. http://dx.doi.org/10.1142/s0218271817410188.

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When quantum gravity effects, that are based on generalized uncertainty principle with a minimal measurable length, are incorporated into black hole physics the Klein–Gordon and Dirac equations get modified. Using these modified equations we investigate tunneling of scalar particles and fermions from event and acceleration horizons of accelerating and rotating black holes and obtain the modified Hawking temperature with quantum gravity effects. We see that Hawking temperature depends on black hole parameters as well as the quantum numbers of emitted fermions. The quantum corrections slow down black hole evaporation and leave a black hole remnant. This contradicts complete evaporation of a black hole which is presaged by the standard temperature formula for black holes. The modified Hawking temperatures presented here, in appropriate limits, are consistent with the previous results in the literature.

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Volovik, G. E. "Effect of the inner horizon on the black hole thermodynamics: Reissner–Nordström black hole and Kerr black hole." Modern Physics Letters A 36, no. 24 (August 10, 2021): 2150177. http://dx.doi.org/10.1142/s0217732321501777.

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For the Schwarzschild black hole, the Bekenstein–Hawking entropy is proportional to the area of the event horizon. For the black holes with two horizons, the thermodynamics is not very clear, since the role of the inner horizons is not well established. Here we calculate the entropy of the Reissner–Nordström black hole and of the Kerr black hole, which have two horizons. For the spherically symmetric Reissner–Nordström black hole, we used several different approaches. All of them give the same result for the entropy and for the corresponding temperature of the thermal Hawking radiation. The entropy is not determined by the area of the outer horizon, and it is not equal to the sum of the entropies of two horizons. It is determined by the correlations between the two horizons, due to which the total entropy of the black hole and the temperature of Hawking radiation depend only on mass M of the black hole and do not depend on the black hole charge Q. For the Kerr and Kerr–Newman black holes, it is shown that their entropy has the similar property: it depends only on mass M of the black hole and does not depend on the angular momentum J and charge Q.

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Addazi, Andrea, and Salvatore Capozziello. "The fate of Schwarzschild–de Sitter black holes in f(R) gravity." Modern Physics Letters A 31, no. 09 (March 21, 2016): 1650054. http://dx.doi.org/10.1142/s0217732316500541.

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The semiclassical effects of anti-evaporating black holes can be discussed in the framework of f(R) gravity. In particular, the Bousso–Hawking–Nojiri–Odinstov anti-evaporation instability of degenerate Schwarzschild–de Sitter black holes (the so-called Nariai spacetime) leads to a dynamical increasing of black hole horizon in f(R) gravity. This phenomenon causes the following transition: emitting marginally trapped surfaces (TS) become space-like surfaces before the effective Bekenstein–Hawking emission time. As a consequence, Bousso–Hawking thermal radiation cannot be emitted in an anti-evaporating Nariai black hole. Possible implications in cosmology and black hole physics are also discussed.

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Hod, Shahar. "Ten shades of black." International Journal of Modern Physics D 24, no. 12 (October 2015): 1544007. http://dx.doi.org/10.1142/s0218271815440071.

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The holographic principle has taught us that, as far as their entropy content is concerned, black holes in (3 + 1)-dimensional curved spacetimes behave as ordinary thermodynamic systems in flat (2 + 1)-dimensional spacetimes. In this paper, we point out that the opposite behavior can also be observed in black-hole physics. To show this we study the quantum Hawking evaporation of near-extremal Reissner–Nordström (RN) black holes. We first point out that the black-hole radiation spectrum departs from the familiar radiation spectrum of genuine (3 + 1)-dimensional perfect black-body emitters. In particular, the would be black-body thermal spectrum is distorted by the curvature potential which surrounds the black-hole and effectively blocks the emission of low-energy quanta. Taking into account the energy-dependent gray-body factors which quantify the imprint of passage of the emitted radiation quanta through the black-hole curvature potential, we reveal that the (3 + 1)-dimensional black holes effectively behave as perfect black-body emitters in a flat (9 + 1)-dimensional spacetime.

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Hussein, N. A., D. A. Eisa, and T. A. S. Ibrahim. "The Free Energy for Rotating and Charged Black Holes and Banados, Teitelboim and Zanelli Black Holes." Zeitschrift für Naturforschung A 73, no. 11 (October 25, 2018): 1061–73. http://dx.doi.org/10.1515/zna-2018-0210.

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AbstractThis paper aims to obtain the thermodynamic variables (temperature, thermodynamic volume, angular velocity, electrostatic potential, and heat capacity) corresponding to the Schwarzschild black hole, Reissner-Nordstrom black hole, Kerr black hole and Kerr-Newman-Anti-de Sitter black hole. We also obtained the free energy for black holes by using three different methods. We obtained the equation of state for rotating Banados, Teitelboim and Zanelli black holes. Finally, we used the quantum correction of the partition function to obtain the heat capacity and entropy in the quantum sense.

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Saghafi, Sara, and Kourosh Nozari. "Black hole thermodynamics in Snyder phase space." International Journal of Geometric Methods in Modern Physics 14, no. 11 (October 23, 2017): 1750164. http://dx.doi.org/10.1142/s021988781750164x.

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By defining a noncommutative symplectic structure, we study thermodynamics of Schwarzschild black hole in a Snyder noncommutative phase space for the first time. Since natural cutoffs are the results of compactness of symplectic manifolds in phase space, the physics of black holes in such a space would be affected mainly by these cutoffs. In this respect, this study provides a basis for more deeper understanding of the black hole thermodynamics in a pure mathematical viewpoint.

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Das, Sumit R., and Samir D. Mathur. "The Quantum Physics of Black Holes: Results from String Theory." Annual Review of Nuclear and Particle Science 50, no. 1 (December 2000): 153–206. http://dx.doi.org/10.1146/annurev.nucl.50.1.153.

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▪ Abstract We review recent progress in our understanding of the physics of black holes. In particular, we discuss the ideas from string theory that explain the entropy of black holes from a counting of microstates of the hole, and the related derivation of unitary Hawking radiation from such holes.

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WHITING, BERNARD F. "NEW RESULTS IN BLACK HOLE PHYSICS." International Journal of Modern Physics D 03, no. 01 (March 1994): 317–21. http://dx.doi.org/10.1142/s021827189400054x.

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Brief statements are given on recent results in the following areas: 1) The derivation of a variational (maximum) principle for black hole entropy, and an outline of the physically reasonable properties of the related solution for the density of states in the microcanonical equilibrium ensemble (with Jeffrey Melmed, University of Maine). 2) Analysis of topological contributions to black hole entropy in Lovelock gravity, and the corresponding thermodynamic identity (with Jonathan Z. Simon, University of Maryland). 3) Stability analysis for a shell of matter surrounding a black hole in microcanonical (thermal) equilibrium (with Gerald Horwitz, Hebrew University, Jerusalem)—results from this work can be compared with an earlier analysis of the purely mechanical stability of the shell, and with known properties of both the dynamical and thermal stability for the black hole without a shell. 4) The study of a simple ‘singularity'-free model of gravitational collapse, and an examination of the relationship between the ensuing preservation of quantum coherence and the usual perception that mixed states should be associated with the late time emission of Hawking radiation from a classically formed black hole (with Gerard ’t Hooft and Chris Stephens, University of Utrecht).

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Martinec, Emil J., and Samson L. Shatashvili. "Black hole physics and Liouville theory." Nuclear Physics B 368, no. 2 (January 1992): 338–58. http://dx.doi.org/10.1016/0550-3213(92)90531-f.

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Åman, Jan, Ingemar Bengtsson, and Narit Pidokrajt. "Thermodynamic Metrics and Black Hole Physics." Entropy 17, no. 12 (September 22, 2015): 6503–18. http://dx.doi.org/10.3390/e17096503.

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de Alwis, S. P. "Black hole physics from Liouville theory." Physics Letters B 300, no. 4 (February 1993): 330–35. http://dx.doi.org/10.1016/0370-2693(93)91341-j.

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González-Díaz, P. F. "On the Black Hole Internal Physics." Annalen der Physik 498, no. 1-2 (1986): 62–66. http://dx.doi.org/10.1002/andp.19864980108.

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GONCHAROV, YU P., and J. V. YAREVSKAYA. "COMPLEX LINE BUNDLES OVER TWO-SPHERE AND BLACK HOLE PHYSICS." Modern Physics Letters A 09, no. 34 (November 10, 1994): 3175–83. http://dx.doi.org/10.1142/s0217732394002999.

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We discuss a long-standing problem of the global topological non-trivial properties of the four-dimensional space-times underlying black hole physics and observe that the standard space-time topology of the ℝ2×S2 form for black hole physics admits topologically inequivalent configurations of a complex scalar field on black hole by virtue of the availability of non-trivial complex line bundles over S2. Each configuration can be labeled by its Chern number n∈ℤ. For the Schwarzschild black hole we formulate an appropriate wave equation for these configurations in massless case and describe its solutions as a first step to study quantum effects for the above configurations within the framework of black hole physics.

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Berezin, Victor. "Black hole thermodynamics without a black hole?" Nuclear Physics B 661, no. 1-2 (June 2003): 409–22. http://dx.doi.org/10.1016/s0550-3213(03)00251-7.

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Liang, Tairan, and Wei Xu. "Leading order of quantum corrections to black hole entropy sum relations." International Journal of Modern Physics A 34, no. 32 (November 20, 2019): 1950216. http://dx.doi.org/10.1142/s0217751x19502166.

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It has been found recently that the entropy relations of horizons have the universality of black hole mass-independence for many black holes. These universal entropy relations have some geometric and CFT understanding, which may provide further insight into the quantum physics of black holes. In this paper, we present the leading order of black hole entropy sum relations under the quantum corrections. It is found that the modified entropy sum becomes mass-dependent for some black holes in asymptotical (A)dS and flat space–times. We also give an example that the modified entropy sum of regular Bardeen AdS black holes is mass-independent, which may be quantized in the form of the electric charge and the cosmological constant.

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Wen, Wen-Yu. "Thermodynamic metric of deformed Schwarzschild black holes." International Journal of Modern Physics D 26, no. 10 (August 20, 2017): 1750106. http://dx.doi.org/10.1142/s0218271817501061.

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Thermodynamic metric usually works only for those black holes with more than one conserved charge, thereby excluding the Schwarzschild black hole. In this paper, however, different versions of thermodynamic metric are computed and compared for the Schwarzschild-like black hole by introducing new degrees of freedom. These new degrees of freedom have two purposes. First, the deformed metric may be treated offshell to the ordinary Schwarzschild black hole, and onshell physics corresponds to the submanifold by gauge fixing of this additional degree of freedom. In particular, the thermal Ricci scalar for the Schwarzschild black hole, though different for various deformations, can be obtained by switching off the deformation. Second, while deformed metric is treated onshell, a divergent Ricci scalar may signal an exotic phase in which new physical degrees of freedom manifest. This paper considers the new degree of freedom as the running Newton constant, a cutoff scale for regular black holes, a noncommutative deformation or the deformed parameter in the nonextensive Tsallis–Rènyi entropy.

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Narzilloev, Bakhtiyor, and Bobomurat Ahmedov. "Observational and Energetic Properties of Astrophysical and Galactic Black Holes." Symmetry 15, no. 2 (January 20, 2023): 293. http://dx.doi.org/10.3390/sym15020293.

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The work reviews the investigation of electromagnetic, optical, and energetic properties of astrophysical and galactic black holes and surrounding matter. The astrophysical applications of the theoretical models of black hole environment to the description of various observed phenomena, such as cosmic rays of the ultra-high-energy, black hole shadow, gravitational lensing, quasinormal modes, jets showing relativistic effects such as the Doppler beaming, thermal radiation from the accretion discs, quasiperiodic oscillations are discussed. It has been demonstrated that the observational data strongly depends on the structure and evolution of the accretion disk surrounding the central black hole. It has been shown that the simulated images of supermassive black holes obtained are in agreement with the observational images obtained by event horizon telescope collaboration. High energetic activity from supermassive black holes due to the magnetic Penrose process discussed in the work is in agreement with the highly energetic cosmic rays observed. The astronomical observation of black holes provides rich fundamental physics laboratories for experimental tests and verification of various models of black hole accretion and different theories of gravity in the regime of strong gravity.

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Murodov, Sardor, Javlon Rayimbaev, Bobomurat Ahmedov, and Eldor Karimbaev. "Quasiperiodic Oscillations and Dynamics of Test Particles around Quasi- and Non-Schwarzschild Black Holes." Universe 9, no. 9 (August 29, 2023): 391. http://dx.doi.org/10.3390/universe9090391.

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One of the open problems in black hole physics is testing spacetime around black holes through astrophysical observations in the strong field regime. In fact, black holes cannot produce radiation themselves in the electromagnetic spectrum. However, a black hole’s gravity plays an important role in the production of the radiation of the accretion disc around it. One may obtain valuable information from the electromagnetic radiation of accretion discs about the gravitational properties of the spacetime around black holes. In this work, we study particle dynamics in the spacetime of quasi- and non-Schwarzschild black holes. We compare the gravitational effects of the spacetime deformation parameters of both black hole solutions on the innermost stable circular orbit (ISCO) radius, position, energy, and angular momentum of test particles at the ISCO, together with the energy efficiency of the accretion disc in the thin Novikov–Thorn model. Furthermore, we study the frequencies of particle oscillations in the radial and angular directions along circular stable orbits around both deformed black holes. Furthermore, we investigate quasiperiodic oscillations around the black holes in the relativistic precession model. We show the dependence of the deviation parameters on the orbits of twin peak QPOs with the frequency ratio 3:2. In the obtained results, we compare the gravitational effects of deviation parameters with the spin of a rotating Kerr black hole. Finally, we obtain constraints on the values of the deviation parameter of the spacetime around the black hole at the center of the microquasars GRO J1655-40 and GRS 1915-105 and their mass, using the χ2 method.

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Chen, Tianyi, Shutong Ge, Jiahui Li, and Xuheng Ma. "The Progress of Black Holes: Principles & Physical Detection Technology." Journal of Physics: Conference Series 2083, no. 2 (November 1, 2021): 022047. http://dx.doi.org/10.1088/1742-6596/2083/2/022047.

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Abstract Humans have been trying to explain black holes since the 19th century, using theoretical understanding and observations of the universe. Incandescent body thermal radiation has been the focus of extensive theoretical and experimental research for over a century. This paper will discuss the concept of a black hole and use information retrieval to generate a panoramic image of it. The content illustrates black holes from three different perspectives: description of black holes using mathematical methods and data, models, and detection. A black hole is a controversial object, and no one knows for sure what it is. Indeed, multiple numerical simulations have been carried out to investigate the critical behaviors of black holes with various geometrical configurations in arbitrary dimensions. We will sum up the black hole knowledge so far and discuss the recent progress in terms of black hole exploration, i.e., shed light for future black holes model construction and detection.

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Braunstein, Samuel L., and Stefano Pirandola. "Quantum information versus black hole physics: deep firewalls from narrow assumptions." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 376, no. 2123 (May 28, 2018): 20170324. http://dx.doi.org/10.1098/rsta.2017.0324.

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The prevalent view that evaporating black holes should simply be smaller black holes has been challenged by the firewall paradox. In particular, this paradox suggests that something different occurs once a black hole has evaporated to one-half its original surface area. Here, we derive variations of the firewall paradox by tracking the thermodynamic entropy within a black hole across its entire lifetime and extend it even to anti-de Sitter space–times. Our approach sweeps away many unnecessary assumptions, allowing us to demonstrate a paradox exists even after its initial onset (when conventional assumptions render earlier analyses invalid). The most natural resolution may be to accept firewalls as a real phenomenon. Further, the vast entropy accumulated implies a deep firewall that goes ‘all the way down’ in contrast with earlier work describing only a structure at the horizon. This article is part of a discussion meeting issue ‘Foundations of quantum mechanics and their impact on contemporary society’.

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Leonhardt, Ulf, and Thomas G. Philbin. "The case for artificial black holes." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 366, no. 1877 (June 5, 2008): 2851–57. http://dx.doi.org/10.1098/rsta.2008.0072.

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The event horizon is predicted to generate particles from the quantum vacuum, an effect that bridges three areas of physics—general relativity, quantum mechanics and thermodynamics. The quantum radiation of real black holes is too feeble to be detectable, but black-hole analogues may probe several aspects of quantum black holes. In this paper, we explain in simple terms some of the motivations behind the study of artificial black holes.

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Schneider, Fabian R. N., Philipp Podsiadlowski, and Eva Laplace. "Bimodal Black Hole Mass Distribution and Chirp Masses of Binary Black Hole Mergers." Astrophysical Journal Letters 950, no. 2 (June 1, 2023): L9. http://dx.doi.org/10.3847/2041-8213/acd77a.

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Abstract In binary black hole mergers from isolated binary-star evolution, both black holes are from progenitor stars that have lost their hydrogen-rich envelopes by binary mass transfer. Envelope stripping is known to affect the pre-supernova core structures of such binary-stripped stars and thereby their final fates and compact remnant masses. In this paper, we show that binary-stripped stars give rise to a bimodal black hole mass spectrum with characteristic black hole masses of about 9 M ⊙ and 16 M ⊙ across a large range of metallicities. The bimodality is linked to carbon and neon burning becoming neutrino dominated, which results in interior structures that are difficult to explode and likely lead to black hole formation. The characteristic black hole masses from binary-stripped stars have corresponding features in the chirp-mass distribution of binary black hole mergers: peaks at about 8 and 14 M ⊙ and a dearth in between these masses. Current gravitational-wave observations of binary black hole mergers show evidence for a gap at 10–12 M ⊙ and peaks at 8 and 14 M ⊙ in the chirp-mass distribution. These features are in agreement with our models of binary-stripped stars. In the future, they may be used to constrain the physics of late stellar evolution and supernova explosions and may even help measure the cosmological expansion of the universe.

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NG, Y. JACK, and H. VAN DAM. "SPACETIME FOAM, HOLOGRAPHIC PRINCIPLE, AND BLACK HOLE QUANTUM COMPUTERS." International Journal of Modern Physics A 20, no. 06 (March 10, 2005): 1328–35. http://dx.doi.org/10.1142/s0217751x05024237.

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Spacetime foam, also known as quantum foam, has its origin in quantum fluctuations of spacetime. Arguably it is the source of the holographic principle, which severely limits how densely information can be packed in space. Its physics is also intimately linked to that of black holes and computation. In particular, the same underlying physics is shown to govern the computational power of black hole quantum computers.

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Liang, Xiao, Zhuo Zhou, and Jiu Hui Wu. "The experimental study on low frequency sound transmission characteristics of the acoustic black hole." Modern Physics Letters B 33, no. 36 (December 19, 2019): 1950458. http://dx.doi.org/10.1142/s021798491950458x.

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The acoustic black hole has good sound insulation performance in low frequency range. The transmission and insulation characteristics of acoustic black hole is investigated by experiments. First, we study the transmission and insulation characteristics of the acoustic black hole by numerical simulation. Second, we studied the sound transmission characteristic of multi-level acoustic black hole. Finally, the sound transmission and insulation characteristics of the acoustic black hole are studied by experiments. The influence of the acoustic black hole tip’s diameter on sound insulation coefficient is studied. The sound transmission characteristics of the first, two and three level acoustic black holes are also studied by experiments. Our numerical results show that low frequency acoustic energy can be effectively focused at the tip of the acoustic black hole, and can be effectively insulated by the acoustic black hole. Our numerical results are verified by the experimental results. Our study can provide a feasible method for controlling the low frequency noise.

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NICOLINI, PIERO. "NONCOMMUTATIVE BLACK HOLES, THE FINAL APPEAL TO QUANTUM GRAVITY: A REVIEW." International Journal of Modern Physics A 24, no. 07 (March 20, 2009): 1229–308. http://dx.doi.org/10.1142/s0217751x09043353.

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We present the state of the art regarding the relation between the physics of Quantum Black Holes and Noncommutative Geometry. We start with a review of models proposed in the literature for describing deformations of General Relativity in the presence of noncommutativity, seen as an effective theory of Quantum Gravity. We study the resulting metrics, proposed to replace or at least to improve the conventional black hole solutions of Einstein's equation. In particular, we analyze noncommutative-inspired solutions obtained in terms of quasiclassical noncommutative coordinates: indeed because of their surprising new features, these solutions enable us to circumvent long standing problems with Quantum Field Theory in Curved Space and to cure the singular behavior of gravity at the centers of black holes. As a consequence, for the first time, we get a complete description of what we may call the black hole SCRAM, the shut down of the emission of thermal radiation from the black hole: in place of the conventional scenario of runaway evaporation in the Planck phase, we find a zero temperature final state, a stable black hole remnant, whose size and mass are determined uniquely in terms of the noncommutative parameter θ. This result turns out to be of vital importance for the physics of the forthcoming experiments at the LHC, where mini black hole production is foreseen in extreme energy hadron collisions. Because of this, we devote the final part of this review to higher-dimensional solutions and their phenomenological implications for TeV Gravity.

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Gao, Zeyuan, and Liu Zhao. "Restricted phase space thermodynamics for AdS black holes via holography." Classical and Quantum Gravity 39, no. 7 (March 11, 2022): 075019. http://dx.doi.org/10.1088/1361-6382/ac566c.

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Abstract A new formalism for thermodynamics of AdS black holes called the restricted phase space thermodynamics (RPST) is proposed. The construction is based on top of Visser’s holographic thermodynamics, but with the AdS radius fixed as a constant. Thus the RPST is free of the (P, V) variables but inherits the central charge and chemical potential as a new pair of conjugate thermodynamic variables. In this formalism, the Euler relation and the Gibbs–Duhem equation hold simultaneously with the first law of black hole thermodynamics, which guarantee the appropriate homogeneous behaviors for the black hole mass and the intensive variables. The formalism is checked in detail in the example case of four-dimensional Reissner–Nordström anti-de Sitter black hole in Einstein–Maxwell theory, in which some interesting thermodynamic behaviors are revealed.

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DANIELSSON, ULF H. "BLACK HOLE UNCERTAINTIES." Modern Physics Letters A 08, no. 20 (June 28, 1993): 1925–41. http://dx.doi.org/10.1142/s0217732393001653.

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In this work the quantum theory of two-dimensional dilaton black holes is studied using the Wheeler-De Witt equation. The solutions correspond to wave functions of the black hole. It is found that for an observer inside the horizon, there are uncertainty relations for the black hole mass and a parameter in the metric determining the Hawking flux. Only for a particular value of this parameter can both be known with arbitrary accuracy. In the generic case there is instead a relation that is very similar to the so-called string uncertainty relation.

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WILCZEK, FRANK. "LECTURES ON BLACK HOLE QUANTUM MECHANICS." International Journal of Modern Physics A 13, no. 31 (December 20, 1998): 5279–372. http://dx.doi.org/10.1142/s0217751x98002420.

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The lectures that follow were originally given in 1992, and written up only slightly later. Since then there have been dramatic developments in the quantum theory of black holes, especially in the context of string theory. None of these are reflected here. The concept of quantum hair, which is discussed at length in the lectures, is certainly of permanent interest, and I continue to believe that in some generalized form it will prove central to the whole question of how information is stored in black holes. The discussion of scattering and emission modes from various classes of black holes could be substantially simplified using modern techniques, and from currently popular perspectives the choice of examples might look eccentric. On the other hand fashions have changed rapidly in the field, and the big questions as stated and addressed here, especially as formulated for "real" black holes (nonextremal, in four-dimensional, asymptotically flat space–time, with supersymmetry broken), remain pertinent even as the tools to address them may evolve. The four lectures I gave at the school were based on two lengthy papers that have now been published, "Black Holes as Elementary Particles," Nuclear PhysicsB380, 447 (1992) and "Quantum Hair on Black Holes," Nuclear PhysicsB378, 175 (1992). The unifying theme of this work is to help make plausible the possibility that black holes, although they are certainly unusual and extreme states of matter, may be susceptible to a description using concepts that are not fundamentally different from those we use in describing other sorts of quantum-mechanical matter. In the first two lectures I discussed dilaton black holes. The fact that apparently innocuous changes in the "matter" action can drastically change the properties of a black hole is already very significant: it indicates that the physical properties of small black holes cannot be discussed reliably in the abstract, but must be considered with due regard to the rest of physics. (The macroscopic properties of large black holes, in particular those of astrophysical interest, are presumably well described by the familiar Einstein–Maxwell action which governs the massless fields. Heavy fields will at most provide Yukawa tails to the field surrounding the hole.) I will show how perturbations may be set up and analyzed completely, and why doing this is crucial for understanding the semiclassical physics of the hole including the Hawking radiation quantitatively. It will emerge that there is a class of dilaton black holes which behave as rather straightforward elementary particles. In the other two lectures I discussed the issue of hair on black holes, in particular the existence of hair associated with discrete gauge charges and its physical consequences. This hair is particularly interesting to analyze because it is invisible classically and to all order in ℏ. Its existence shows that black holes can have some "internal" quantum numbers in addition to their traditional classification by mass, charge, and angular momentum. The text that follows, follows the original papers closely.

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Nielsen, Alex B. "Black holes and black hole thermodynamics without event horizons." General Relativity and Gravitation 41, no. 7 (January 16, 2009): 1539–84. http://dx.doi.org/10.1007/s10714-008-0739-9.

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Zomorrodian, Mohammad Ebrahim, Alireza Sepehri, and Aliakbar Moradi Marjaneh. "The information loss for QCD matter in mini black holes at LHC." Canadian Journal of Physics 88, no. 11 (November 2010): 841–49. http://dx.doi.org/10.1139/p10-064.

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In this paper we find information loss in mini black holes at LHC by extending the Horowitz and Maldacena mechanism to gluons and calculate the information transformation from the collapsing matter to the state of outgoing Hawking radiation for gluons, quarks, and mesons. Next, we calculate the total cross-section for mesons produced from black holes at LHC. We conclude that the more the mass of the quark within the hadrons, the lower is the cross-section. Then, we consider the effect of quarks inside the black hole on the density matrix of individual quarks within the meson outside of a black hole. At the end, we show that information is not lost in black holes if we ignore interactions between particles inside the event horizon in comparison with the effect of a black hole on particles. However, we observe that the unstable condition of excited black holes causes information loss in them. After that, we anticipate quantum black hole production by using electron–positron annihilation modeling at TeV centre of mass energies and compare the corresponding cross-sections calculated, at this stage, for different black hole states. Finally, we calculate the dependence of gluon tree level amplitudes to their thermal distributions near mini black holes at LHC.

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Du, Yun-Zhi, Hui-Hua Zhao, and Li-Chun Zhang. "Phase Transition of the Horava-Lifshitz AdS Black Holes." International Journal of Theoretical Physics 60, no. 5 (April 28, 2021): 1963–71. http://dx.doi.org/10.1007/s10773-021-04814-z.

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AbstractSome ones have showed the first-order phase transition of the Horava-Lifshitz (HL) AdS black holes has unique characters from other AdS black holes. While the coexistence zone of the first-order phase transition was not exhibited. As well known the coexistence curve of a black hole carries a lot of information about black hole, which provides a powerful diagnostic of the thermodynamic properties on black hole. We study the first-order phase transition coexistence curves of the HL AdS black holes by the Maxwell’s equal-area law, and give the boundary of two-phase coexistence zone. It is very interesting that the first-order phase transition point is determined by the pressure F on the surface of the HL AdS black hole’s horizon, instead of only the pressure P (or the temperature T). This unique property distinguishes the HL AdS black hole from the other AdS black hole systems. Furthermore, this black hole system have the critical curves, and on which every point stands for a critical point.

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Kenath, Arun, Samartha C. A., and K. A. Chrandrashekaran. "Kerr Black Holes and Jets." Mapana - Journal of Sciences 4, no. 2 (August 15, 2005): 67–74. http://dx.doi.org/10.12723/mjs.7.8.

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during the sen*ster M.E. under the guidance of Prof. C Sivarorn, We are very thankful to Prof. C. for his guidance out and hoi. K. A Q•androshekor, H. O O, PG Dept Physics. Christ for and encouragement. Black holes A is a of pace-time that rTWSS in it that there is no way for a nearby object iO escape its gravitational pun. Since Our best thory of gravity Of the moment is Einstein' s general theory oi relativity, we have delve into some results Of this theory to understand black holes in The basic associated With 0 block hole is its Schwarzschild radius.

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Buchanan, Mark. "Black Hole Assembly Line." Physics 12 (November 1, 2019). http://dx.doi.org/10.1103/physics.12.120.

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Kocherlakota, Prashant, and Luciano Rezzolla. "Distinguishing gravitational and emission physics in black hole imaging: spherical symmetry." Monthly Notices of the Royal Astronomical Society, April 1, 2022. http://dx.doi.org/10.1093/mnras/stac891.

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Abstract Imaging a supermassive black hole and extracting physical information requires good knowledge of both the gravitational and the astrophysical conditions near the black hole. When the geometrical properties of the black hole are well understood, extracting information on the emission properties is possible. Similarly, when the emission properties are well understood, extracting information on the black hole geometry is possible. At present however, uncertainties are present both in the geometry and in the emission, and this inevitably leads to degeneracies in the interpretation of the observations. We explore here the impact of varying geometry and emission coefficient when modelling the imaging of a spherically-accreting black hole. Adopting the Rezzolla-Zhidenko parametric metric to model arbitrary static black-holes, we first demonstrate how shadow-size measurements leave degeneracies in the multidimensional space of metric-deviation parameters, even in the limit of infinite-precision measurements. Then, at finite precision, we show that these degenerate regions can be constrained when multiple pieces of information, such as the shadow-size and the peak image intensity contrast, are combined. Such degeneracies can potentially be eliminated with measurements at increased angular-resolution and flux-sensitivity. While our approach is restricted to spherical symmetry and hence idealised, we expect our results to hold also when more complex geometries and emission processes are considered.

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McCormick, Katie. "Ionizing Black Hole “Atoms”." Physics 15 (June 2, 2022). http://dx.doi.org/10.1103/physics.15.s74.

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Wong, George N. "Measuring a Black Hole Shadow." Physics 15 (May 9, 2022). http://dx.doi.org/10.1103/physics.15.68.

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Journal articles on the topic 'Black hole physics'

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