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Articoli di riviste sul tema "Radiation de Hawking acoustique"

Autore: Grafiati

Pubblicato: 25 gennaio 2025

Ultima modifica: 31 luglio 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 (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 (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 (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 (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 (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 (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 (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 (1987): 1065–79. http://dx.doi.org/10.1103/physrevd.36.1065.

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11

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 (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 identi

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12

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 (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

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13

Qadir, Asghar. "On the reality of Hawking radiation." International Journal of Modern Physics D 28, no. 16 (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 real

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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 (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 evapora

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15

Wang, Jingbo. "Hawking Radiation from the Boundary Scalar Field and the Information Loss Paradox." Universe 9, no. 3 (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 se

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16

VOLOVIK, G. E. "ON DE SITTER RADIATION VIA QUANTUM TUNNELING." International Journal of Modern Physics D 18, no. 08 (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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17

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 (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

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18

MODAK, SUJOY KUMAR, and DOUGLAS SINGLETON. "HAWKING RADIATION AS A MECHANISM FOR INFLATION." International Journal of Modern Physics D 21, no. 11 (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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19

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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20

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

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21

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

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22

Harikumar, E., та N. S. Zuhair. "Hawking radiation in κ-spacetime". International Journal of Modern Physics A 32, № 13 (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]-def

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23

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

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24

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

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25

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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26

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

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27

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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28

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

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29

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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30

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

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31

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

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32

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

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Abstract (sommario):

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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33

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

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34

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

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35

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

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36

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

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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 (2020): 2043019. http://dx.doi.org/10.1142/s0218271820430191.

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Abstract (sommario):

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 singular

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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 (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 (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

Ho, Pei-Ming. "From uneventful Horizon to firewall in D-dimensional effective theory." International Journal of Modern Physics A 36, no. 19 (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 horizo

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41

CHEN, DEYOU, and SHUZHENG YANG. "A METHOD TO STUDY THE HAWKING RADIATION OF THE KERR BLACK HOLE." Modern Physics Letters A 22, no. 34 (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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42

HOTTA, M., and M. YOSHIMURA. "END POINT OF HAWKING EVAPORATION — CASE OF INTEGRABLE MODEL." Modern Physics Letters A 09, no. 18 (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 co

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43

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 (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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44

Chen, Pisin, Gerard Mourou, Marc Besancon, et al. "AnaBHEL (Analog Black Hole Evaporation via Lasers) Experiment: Concept, Design, and Status." Photonics 9, no. 12 (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 a

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45

Marto, João. "Hawking Radiation and Black Hole Gravitational Back Reaction—A Quantum Geometrodynamical Simplified Model." Universe 7, no. 8 (2021): 297. http://dx.doi.org/10.3390/universe7080297.

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The purpose of this paper is to analyse the back reaction problem, between Hawking radiation and the black hole, in a simplified model for the black hole evaporation in the quantum geometrodynamics context. The idea is to transcribe the most important characteristics of the Wheeler-DeWitt equation into a Schrödinger’s type of equation. Subsequently, we consider Hawking radiation and black hole quantum states evolution under the influence of a potential that includes back reaction. Finally, entropy is estimated as a measure of the entanglement between the black hole and Hawking radiation states

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46

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 (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 char

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47

VISSER, MATT. "HAWKING RADIATION: A PARTICLE PHYSICS PERSPECTIVE." Modern Physics Letters A 08, no. 18 (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

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48

Zhang, Wen-Jie, Pu-Jian Mao, and Jun-Bao Wu. "Hawking radiation of Dirac particles from soft-hairy black holes." Communications in Theoretical Physics 74, no. 4 (2022): 045401. http://dx.doi.org/10.1088/1572-9494/ac588e.

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Abstract In this paper, we study the Hawking radiation of Dirac particles via tunneling formalism from linearly supertranslated Schwarzschild black holes. We find that the radiation spectrum and the Hawking temperature remain the same as the one without soft hair.

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49

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

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Abstract (sommario):

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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50

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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Abstract (sommario):

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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