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Journal articles on the topic 'Radiation de Hawking acoustique'

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Published: 25 January 2025

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1

Spindel, Renaud. "Hawking radiation." Scholarpedia 6, no. 12 (2011): 6958. http://dx.doi.org/10.4249/scholarpedia.6958.

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2

Carusotto, Iacopo, and Roberto Balbinot. "Acoustic Hawking radiation." Nature Physics 12, no. 10 (August 15, 2016): 897–98. http://dx.doi.org/10.1038/nphys3872.

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3

Sakalli, I., and A. Ovgun. "Uninformed Hawking radiation." EPL (Europhysics Letters) 110, no. 1 (April 1, 2015): 10008. http://dx.doi.org/10.1209/0295-5075/110/10008.

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4

Sakalli, Izzet, Mustafa Halilsoy, and Hale Pasaoglu. "Fading Hawking radiation." Astrophysics and Space Science 340, no. 1 (February 29, 2012): 155–60. http://dx.doi.org/10.1007/s10509-012-1028-3.

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5

Irani, Ardeshir. "Cherenkov Radiation and Hawking Radiation." Open Journal of Philosophy 14, no. 03 (2024): 623–27. http://dx.doi.org/10.4236/ojpp.2024.143042.

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6

Hotta, M., and M. Yoshimura. "Wormhole and Hawking Radiation." Progress of Theoretical Physics 91, no. 1 (January 1, 1994): 181–86. http://dx.doi.org/10.1143/ptp/91.1.181.

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7

Blau, Stephen K. "Hawking radiation from fluids." Physics Today 67, no. 12 (December 2014): 23. http://dx.doi.org/10.1063/pt.3.2613.

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8

Kiefer, Claus. "Hawking radiation from decoherence." Classical and Quantum Gravity 18, no. 22 (November 2, 2001): L151—L154. http://dx.doi.org/10.1088/0264-9381/18/22/101.

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9

Parikh, Maulik K., and Frank Wilczek. "Hawking Radiation As Tunneling." Physical Review Letters 85, no. 24 (December 11, 2000): 5042–45. http://dx.doi.org/10.1103/physrevlett.85.5042.

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10

Hajicek, Petr. "Origin of Hawking radiation." Physical Review D 36, no. 4 (August 15, 1987): 1065–79. http://dx.doi.org/10.1103/physrevd.36.1065.

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11

Aguero-Santacruz, Raul, and David Bermudez. "Hawking radiation in optics and beyond." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 378, no. 2177 (July 20, 2020): 20190223. http://dx.doi.org/10.1098/rsta.2019.0223.

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Hawking radiation was originally proposed in astrophysics, but it has been generalized and extended to other physical systems receiving the name of analogue Hawking radiation. In the last two decades, several attempts have been made to measure it in a laboratory, and one of the most successful systems is in optics. Light interacting in a dielectric material causes an analogue Hawking effect, in fact, its stimulated version has already been detected and the search for the spontaneous signal is currently ongoing. We briefly review the general derivation of Hawking radiation, then we focus on the optical analogue and present some novel numerical results. Finally, we call for a generalization of the term Hawking radiation. This article is part of a discussion meeting issue ‘The next generation of analogue gravity experiments’.
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12

Qadir, Asghar. "On the reality of Hawking radiation." International Journal of Modern Physics D 28, no. 16 (October 11, 2019): 2040001. http://dx.doi.org/10.1142/s0218271820400015.

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Hawking radiation caught the imagination of the public and physicists alike, because it seemed so counter-intuitive. By their very definition, black holes were supposed to endlessly absorb, but never emit, matter and energy. Yet, Hawking argued that taking Quantum Theory into account, they would radiate. The further belief was that Bekenstein and Hawking had developed the field of Black Hole Thermodynamics. Here I want to correct this impression and give due credit to Roger Penrose for founding the subject. Further, I discuss the question of whether Hawking radiation should be expected to really exist, arguing that there is reason to doubt it.
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13

Wen, Peng, Xin-Yang Wang, and Wen-Biao Liu. "The entropy evolution of a noncommutative black hole under Hawking radiation." International Journal of Modern Physics A 35, no. 30 (October 23, 2020): 2050194. http://dx.doi.org/10.1142/s0217751x20501948.

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By calculating the entropy of a scalar field in the interior volume of noncommutative black holes and considering an infinitesimal process of Hawking radiation, a proportion function is constructed that reflects the evolution relation between the scalar field entropy and Bekenstein–Hawking entropy under Hawking radiation. Comparing with the case of Schwarzschild black holes, the new physics of this research can be expanded to the later stage of Hawking radiation. From the result, we find that the proportion function is still a constant in the earlier stage of Hawking radiation, which is identical to the case of Schwarzschild black holes. As Hawking radiation goes into the later stage, the behavior of the function will be dominated by the noncommutative effect. In this circumstance, the proportion function is no longer a constant and decreases with the evaporation process. When the noncommutative black hole evolves into its final state with Hawking radiation, the interior volume will converge to a certain value, which implies that the loss of information of the black hole during the evaporation process will finally be stored in the limited interior volume.
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14

Guo, Chunyu. "The principle and state-of-art applications of Hawking radiation." Journal of Physics: Conference Series 2364, no. 1 (November 1, 2022): 012054. http://dx.doi.org/10.1088/1742-6596/2364/1/012054.

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Abstract Hawking radiation, firstly discovered in 1974 by Stephen Hawking, is a crucial quantum phenomenon, which proves that a black hole has been losing its mass since its formation. In this paper, the method of information retrieval and literature analysis are fully applied to introduce the principle and state-of-art applications of Hawking radiation. Three parameters used to describe the evaporation of black holes are analyzed. Furthermore, the tunnelling effect of entangled pairs near event horizon is described to explain Hawking radiation from a microscopic perspective. Then, the evaporating black holes are observed under wave optical conditions by the Fourier transformation of the spatial correlation function and detected in Laboratory condition by equivalenting entangled pairs to surface wave packets with sum-zero energy. Finally, a prediction is made that the widely used of extra-dimensional theory and high-energy particle technology as well as numerical researches in laboratory conditions will be strongly pushing the observation of Hawking radiation. Overall, these results shed light on further exploring the universe in terms of Hawking radiation.
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15

VOLOVIK, G. E. "ON DE SITTER RADIATION VIA QUANTUM TUNNELING." International Journal of Modern Physics D 18, no. 08 (August 2009): 1227–41. http://dx.doi.org/10.1142/s0218271809015035.

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We discuss why the tunneling picture does not necessarily lead to Hawking radiation from the de Sitter horizon. The experience with the condensed matter analogs of the event horizon suggests that the de Sitter vacuum is stable against Hawking radiation. On the other hand, the detector immersed in the de Sitter background will detect the radiation, which looks thermal, with the effective temperature twice as large as the Hawking temperature associated with the cosmological horizon.
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16

Ibungochouba Singh, T., Y. Kenedy Meitei, and I. Ablu Meitei. "Effect of GUP on Hawking radiation of BTZ black hole." International Journal of Modern Physics A 35, no. 05 (February 20, 2020): 2050018. http://dx.doi.org/10.1142/s0217751x20500189.

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The Hawking radiation of BTZ black hole is investigated based on generalized uncertainty principle effect by using Hamilton–Jacobi method and Dirac equation. The tunneling probability and the Hawking temperature of the spin-1/2 particles of the BTZ black hole are investigated using the modified Dirac equation based on the GUP. The modified Hawking temperature for fermion crossing the black hole horizon includes the mass parameter of the black hole, angular momentum, energy and also outgoing mass of the emitted particle. Besides, considering the effect of GUP into account, the modified Hawking radiation of massless particle from a BTZ black hole is investigated using Damour and Ruffini method, tortoise coordinate transformation and modified Klein–Gordon equation. The relation between the modified Hawking temperature obtained by using Damour–Ruffini method and the energy of the emitted particle is derived. The original Hawking temperature is also recovered in the absence of quantum gravity effect. There is a possibility of negative Hawking temperature for emission of Dirac particles under quantum gravity effects.
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17

Zhao Ren, Zhang Li-Chun, and Li Huai-Fan. "Hawking radiation of black hole." Acta Physica Sinica 57, no. 12 (2008): 7463. http://dx.doi.org/10.7498/aps.57.7463.

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18

Fitzgerald, Richard J. "Tabletop measurements of Hawking radiation." Physics Today 64, no. 3 (March 2011): 22. http://dx.doi.org/10.1063/1.3604511.

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19

Peltola, Ari. "Local approach to Hawking radiation." Classical and Quantum Gravity 26, no. 3 (January 16, 2009): 035014. http://dx.doi.org/10.1088/0264-9381/26/3/035014.

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20

Harikumar, E., and N. S. Zuhair. "Hawking radiation in κ-spacetime." International Journal of Modern Physics A 32, no. 13 (May 5, 2017): 1750072. http://dx.doi.org/10.1142/s0217751x17500725.

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In this paper, we analyze the Hawking radiation of a [Formula: see text]-deformed-Schwarzschild black hole and obtain the deformed Hawking temperature. For this, we first derive deformed metric for the [Formula: see text]-spacetime, which in the generic case, is not a symmetric tensor and also has a momentum dependence. We show that the Schwarzschild metric obtained in the [Formula: see text]-deformed spacetime has a dependence on energy. We use the fact that the deformed metric is conformally flat in the 1[Formula: see text]+[Formula: see text]1 dimensions to solve the [Formula: see text]-deformed Klein–Gordon equation in the background of the Schwarzschild metric. The method of Bogoliubov coefficients is then used to calculate the thermal spectrum of [Formula: see text]-deformed-Schwarzschild black hole and show that the Hawking temperature is modified by the noncommutativity of the [Formula: see text]-spacetime.
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21

Bose, Sukanta, Leonard Parker, and Yoav Peleg. "Hawking Radiation and Unitary Evolution." Physical Review Letters 76, no. 6 (February 5, 1996): 861–64. http://dx.doi.org/10.1103/physrevlett.76.861.

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22

Hambli, N., and C. P. Burgess. "Hawking radiation and ultraviolet regulators." Physical Review D 53, no. 10 (May 15, 1996): 5717–22. http://dx.doi.org/10.1103/physrevd.53.5717.

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23

Han, Jiaqi. "Research Methods of Hawking Radiation." Journal of Physics: Conference Series 1634 (September 2020): 012097. http://dx.doi.org/10.1088/1742-6596/1634/1/012097.

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24

Gangopadhyay, Sunandan. "Anomalies, horizons and Hawking radiation." EPL (Europhysics Letters) 85, no. 1 (January 2009): 10004. http://dx.doi.org/10.1209/0295-5075/85/10004.

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25

Ryskin, Gregory. "Boltzmann factor and Hawking radiation." Physics Letters B 734 (June 2014): 394–95. http://dx.doi.org/10.1016/j.physletb.2014.05.085.

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26

Susskind, Leonard, and Lárus Thorlacius. "Hawking radiation and back-reaction." Nuclear Physics B 382, no. 1 (August 1992): 123–47. http://dx.doi.org/10.1016/0550-3213(92)90081-l.

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27

Wen, Wen-Yu. "Hawking radiation as stimulated emission." Physics Letters B 803 (April 2020): 135348. http://dx.doi.org/10.1016/j.physletb.2020.135348.

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28

Vilkovisky, G. A. "Backreaction of the Hawking radiation." Physics Letters B 638, no. 5-6 (July 2006): 523–25. http://dx.doi.org/10.1016/j.physletb.2006.05.087.

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29

Das, Sumit R. "Hawking radiation in string theory." Journal of Astrophysics and Astronomy 20, no. 3-4 (December 1999): 131–48. http://dx.doi.org/10.1007/bf02702348.

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30

Yoon, Youngsub. "Maxwell–Boltzmann type Hawking radiation." Modern Physics Letters A 32, no. 12 (April 9, 2017): 1750071. http://dx.doi.org/10.1142/s0217732317500717.

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Twenty years ago, Rovelli proposed that the degeneracy of black hole (i.e. the exponential of the Bekenstein–Hawking entropy) is given by the number of ways the black hole horizon area can be expressed as a sum of unit areas. However, when counting the sum, one should treat the area quanta on the black hole horizon as distinguishable. This distinguishability of area quanta is noted in Rovelli’s paper. Building on this idea, we derive that the Hawking radiation spectrum is not given by Planck radiation spectrum (i.e. Bose–Einstein distribution) but given by Maxwell–Boltzmann distribution.
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31

Russo, Jorge G., Leonard Susskind, and Lárus Thorlacius. "End point of Hawking radiation." Physical Review D 46, no. 8 (October 15, 1992): 3444–49. http://dx.doi.org/10.1103/physrevd.46.3444.

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32

Sakagami, M. a., and A. Ohashi. "Hawking Radiation in the Laboratory." Progress of Theoretical Physics 107, no. 6 (June 1, 2002): 1267–72. http://dx.doi.org/10.1143/ptp.107.1267.

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33

Salehi, H. "Hawking radiation and Planck scales." Classical and Quantum Gravity 10, no. 3 (March 1, 1993): 595–604. http://dx.doi.org/10.1088/0264-9381/10/3/018.

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34

Unruh, W. G. "Has Hawking Radiation Been Measured?" Foundations of Physics 44, no. 5 (March 14, 2014): 532–45. http://dx.doi.org/10.1007/s10701-014-9778-0.

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35

Wang, Jingbo. "Hawking Radiation from the Boundary Scalar Field and the Information Loss Paradox." Universe 9, no. 3 (March 18, 2023): 154. http://dx.doi.org/10.3390/universe9030154.

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Hawking radiation is an essential property of the quantum black hole. It results in the information loss paradox and provides an important clue with regard to the unification of quantum mechanics and general relativity. In previous work, the boundary scalar fields on the horizon of black holes were used to determine the microstates of BTZ black holes and Kerr black holes. They account for Bekenstein–Hawking entropy. In this paper, we show that the Hawking radiation can also be derived from those scalar fields. Hawking radiation is a mixture of the thermal radiation of right- and left-moving sectors at different temperatures. Based on this result, for static BTZ black holes and Schwarzschild black holes, we propose a simple solution for the information loss paradox; i.e., the Hawking radiation is pure due to its entanglement between the left-moving sector and the right-moving sector. This entanglement may be detected in an analogue black hole in the near future.
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36

MODAK, SUJOY KUMAR, and DOUGLAS SINGLETON. "HAWKING RADIATION AS A MECHANISM FOR INFLATION." International Journal of Modern Physics D 21, no. 11 (October 2012): 1242020. http://dx.doi.org/10.1142/s0218271812420205.

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The Friedman–Robertson–Walker (FRW) spacetime exhibits particle creation similar to Hawking radiation of a black hole. In this essay we show that this FRW Hawking radiation leads to an effective negative pressure fluid which can drive an inflationary period of exponential expansion in the early universe. Since the Hawking temperature of the FRW spacetime decreases as the universe expands this mechanism naturally turns off and the inflationary stage transitions to a power law expansion associated with an ordinary radiation-dominated universe.
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37

Gan, Wen-Cong, and Fu-Wen Shu. "Information loss paradox revisited: Farewell firewall?" International Journal of Modern Physics D 29, no. 14 (September 24, 2020): 2043019. http://dx.doi.org/10.1142/s0218271820430191.

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Unitary evolution makes pure state on one Cauchy surface evolve to pure state on another Cauchy surface. Outgoing Hawking radiation is the only subsystem on the late Cauchy surface. The requirement that Hawking radiation should be pure amounts to requiring purity of the subsystem when the total system is pure. We will see that this requirement will lead to firewall even in flat spacetime, and thus is invalid. Information is either stored in the entanglement between field modes inside black hole and the outgoing modes or stored in correlation between geometry and Hawking radiation when singularity is resolved by quantum gravity effects. We will give a simple argument that even in semi-classical regime, information is (at least partly) stored in correlation between geometry and Hawking radiation.
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38

Addazi, Andrea. "Suppression of Bekenstein–Hawking radiation in f(T)-gravity." International Journal of Modern Physics A 33, no. 01 (January 10, 2018): 1850001. http://dx.doi.org/10.1142/s0217751x1850001x.

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We discuss semiclassical Nariai black holes in the framework of f(T)-gravity. For a diagonal choice of tetrads, stable Nariai metrics can be found, emitting Bekenstein–Hawking radiation in semiclassical limit. However, for a nondiagonal choice of tetrads, evaporation and anti-evaporation instabilities are turned on. In turn, this causes a backreaction effect suppressing the Bekenstein–Hawking radiation. In particular, evaporation instabilities produce a new radiation — different by Bekenstein–Hawking emission — nonviolating unitarity in particle physics sector.
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39

CHEN, DEYOU, and SHUZHENG YANG. "HAMILTON–JACOBI ANSATZ TO STUDY THE HAWKING RADIATION OF KERR–NEWMAN–KASUYA BLACK HOLES." International Journal of Modern Physics A 22, no. 28 (November 10, 2007): 5173–78. http://dx.doi.org/10.1142/s0217751x07038207.

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Taking the self-gravitation interaction and unfixed background space–time into account, we study the Hawking radiation of Kerr–Newman–Kasuya black holes using Hamilton–Jacobi method. The result shows that the tunneling rate is related to the change of Bekenstein–Hawking entropy and the radiation spectrum deviates from the purely thermal one, which is accordant with that obtained using Parikh and Wilczek's method and gives a correction to the Hawking radiation of the black hole.
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40

CHEN, DE-YOU, and XIAO-TAO ZU. "HAWKING RADIATION OF FERMIONS FOR THE KERR–SEN DILATON–AXION BLACK HOLE." Modern Physics Letters A 24, no. 14 (May 10, 2009): 1159–65. http://dx.doi.org/10.1142/s0217732309027133.

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Recent research on Hawking radiations of the Rindler spacetime and spherically symmetric uncharged spacetime shows that the Hawking temperature can be obtained by fermions tunnelling method. In this paper, we extend this work to the charged rotating spacetime and review the Hawking radiation of the Kerr–Sen dilaton–axion black hole by fermions tunnelling. The Hawking temperature is recovered and is exactly the same as that obtained by other methods.
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41

Ho, Pei-Ming. "From uneventful Horizon to firewall in D-dimensional effective theory." International Journal of Modern Physics A 36, no. 19 (July 3, 2021): 2150145. http://dx.doi.org/10.1142/s0217751x21501451.

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Assuming the standard effective-field-theoretic formulation of Hawking radiation, we show explicitly how a generic effective theory predicts a firewall from an initially uneventful horizon for a spherically symmetric, uncharged black hole in [Formula: see text] dimensions for [Formula: see text]. The firewall is created via higher-derivative interactions within the scrambling time after the collapsing matter enters the trapping horizon. This result manifests the trans-Planckian problem of Hawking radiation and demonstrates the incompatibility between Hawking radiation and the uneventful horizon.
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42

CHEN, DEYOU, and SHUZHENG YANG. "A METHOD TO STUDY THE HAWKING RADIATION OF THE KERR BLACK HOLE." Modern Physics Letters A 22, no. 34 (November 10, 2007): 2611–16. http://dx.doi.org/10.1142/s0217732307022682.

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Using the Hamilton–Jacobi method, we discuss the Hawking radiation of the Kerr black hole. The result shows when the self-gravitational interaction as well as the conservation of energy and angular momentum are taken into account, the radiation spectrum deviates from the purely thermal one and the tunneling probability is related to the change of Bekenstein–Hawking entropy, which is in accordance with Parikh and Wilczek's result and gives a method to study the Hawking radiation of the black hole.
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43

HOTTA, M., and M. YOSHIMURA. "END POINT OF HAWKING EVAPORATION — CASE OF INTEGRABLE MODEL." Modern Physics Letters A 09, no. 18 (June 14, 1994): 1617–26. http://dx.doi.org/10.1142/s0217732394001453.

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Quantum back reaction due to N massless fields may be worked out to a considerable detail in a variant of integrable dilaton gravity model in two dimensions. It is shown that there exists a critical mass of collapsing object of order ħN×(cosmological constant)1/2, above which the end point of Hawking evaporation is two disconnected remnants of infinite extent, each separated by a mouth from the outside region. Deep inside the mouth there is a universal flux of radiation in all directions, in a form different from Hawking radiation. Below the critical mass no remnant is left behind, implying complete Hawking evaporation or even showing no sign of Hawking radiation.
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44

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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45

Nach, M. "Hawking’s radiation of sine–Gordon black holes in two dimensions." International Journal of Modern Physics A 34, no. 16 (June 10, 2019): 1950086. http://dx.doi.org/10.1142/s0217751x19500866.

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In the framework of the integrable model of the sine–Gordon equation, we describe a recent method to recover the Hawking temperature from the sine–Gordon black hole (sGBH). We present the SGBH metric, its event horizon and give the Hawking temperature of sine–Gordon black hole. We use the complex path analysis method to examine the Hawking radiation and give the possibility of estimating the evaporation time of the SGBH.
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46

Chen, Pisin, Gerard Mourou, Marc Besancon, Yuji Fukuda, Jean-Francois Glicenstein, Jiwoo Nam, Ching-En Lin, et al. "AnaBHEL (Analog Black Hole Evaporation via Lasers) Experiment: Concept, Design, and Status." Photonics 9, no. 12 (December 19, 2022): 1003. http://dx.doi.org/10.3390/photonics9121003.

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Accelerating relativistic mirrors have long been recognized as viable settings where the physics mimic those of the black hole Hawking radiation. In 2017, Chen and Mourou proposed a novel method to realize such a system by traversing an ultra-intense laser through a plasma target with a decreasing density. An international AnaBHEL (Analog Black Hole Evaporation via Lasers) collaboration was formed with the objectives of observing the analog Hawking radiation, shedding light on the information loss paradox. To reach these goals, we plan to first verify the dynamics of the flying plasma mirror and characterize the correspondence between the plasma density gradient and the trajectory of the accelerating plasma mirror. We will then attempt to detect the analog Hawking radiation photons and measure the entanglement between the Hawking photons and their “partner particles”. In this paper, we describe our vision and strategy of AnaBHEL using the Apollon laser as a reference, and we report on the progress of our R&D concerning the key components in this experiment, including the supersonic gas jet with a graded density profile, and the superconducting nanowire single-photon Hawking detector. In parallel to these hardware efforts, we performed computer simulations to estimate the potential backgrounds, and derived analytic expressions for modifications to the blackbody spectrum of the Hawking radiation for a perfectly reflecting point mirror, due to the semi-transparency and finite-size effects specific to flying plasma mirrors. Based on this more realistic radiation spectrum, we estimate the Hawking photon yield to guide the design of the AnaBHEL experiment, which appears to be achievable.
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47

Li, Hui Ling, Cheng Cheng, and Yan Ge Wu. "Tunneling Radiation from the Cosmological Horizon." Advanced Materials Research 647 (January 2013): 918–22. http://dx.doi.org/10.4028/www.scientific.net/amr.647.918.

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Extending the Parikh’s method of quantum tunneling radiation, Hawking radiation via tunneling from the cosmological horizon of NUT-Kerr-Newman de Sitter black hole is deeply studied. The result shows that the tunneling rate on the cosmological horizon is related to the change of Bekenstein-Hawking entropy and the real spectrum is not strictly thermal at all, but is consistent with an underlying unitary theory.
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48

VAGENAS, ELIAS C. "TWO-DIMENSIONAL DILATONIC BLACK HOLES AND HAWKING RADIATION." Modern Physics Letters A 17, no. 10 (March 28, 2002): 609–18. http://dx.doi.org/10.1142/s0217732302006862.

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Hawking radiation emanating from two-dimensional charged and uncharged dilatonic black holes — dimensionally reduced from (2+1) spinning and spinless, respectively, BTZ black holes — is viewed as a tunneling process. Two-dimensional dilatonic black holes (AdS(2) included) are treated as dynamical background in contrast to the standard methodology where the background geometry is fixed when evaluating Hawking radiation. This modification to the geometry gives rise to a nonthermal part in the radiation spectrum. Nonzero temperature of the extremal two-dimensional charged black hole is found. The Bekenstein–Hawking area formula is easily derived for these dynamical geometries.
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49

Nikolić, Hrvoje. "Black Hole Information Paradox without Hawking Radiation." Universe 9, no. 1 (December 23, 2022): 11. http://dx.doi.org/10.3390/universe9010011.

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By entangling soft massless particles, one can create an arbitrarily large amount of entanglement entropy that carries an arbitrarily small amount of energy. By dropping this entropy into the black hole (b.h.), one can increase the b.h. entropy by an amount that violates the Bekenstein bound or any other reasonable bound, leading to a version of the b.h. information paradox that does not involve Hawking radiation. Among the many proposed solutions for the standard b.h. information paradox with Hawking radiation, only a few can also resolve this version without Hawking radiation. The assumption that both versions should be resolved in the same way significantly helps to reduce the number of possible resolutions.
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50

Matsuno, Ken. "Hawking radiation of scalar particles and fermions from squashed Kaluza–Klein black holes based on a generalized uncertainty principle." Classical and Quantum Gravity 39, no. 7 (March 11, 2022): 075022. http://dx.doi.org/10.1088/1361-6382/ac4c05.

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Abstract We study the Hawking radiation from the five-dimensional charged static squashed Kaluza–Klein black hole by the tunneling of charged scalar particles and charged fermions. In contrast to the previous studies of Hawking radiation from squashed Kaluza–Klein black holes, we consider the phenomenological quantum gravity effects predicted by the generalized uncertainty principle with the minimal measurable length. We derive corrections of the Hawking temperature to general relativity, which are related to the energy of the emitted particle, the size of the compact extra dimension, the charge of the black hole and the existence of the minimal length in the squashed Kaluza–Klein geometry. We obtain some known Hawking temperatures in five and four-dimensional black hole spacetimes by taking limits in the modified temperature. We show that the generalized uncertainty principle may slow down the increase of the Hawking temperature due to the radiation, which may lead to the thermodynamic stable remnant of the order of the Planck mass after the evaporation of the squashed Kaluza–Klein black hole. We also find that the sparsity of the Hawking radiation modified by the generalized uncertainty principle may become infinite when the mass of the squashed Kaluza–Klein black hole approaches its remnant mass.
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