Information loss and entropy conservation in quantum corrected Hawking radiation

Chen, Yixin; Shao, Kai-Nan

doi:10.1016/j.physletb.2009.06.004

Cited by 43 publications

(50 citation statements)

References 52 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Among various models of black hole radiation, the tunneling model proposed by Parikh and Wilczek [21] has provided useful insights in the effort to resolve the information loss paradox [22], black hole evolution [23,24], and black hole remnants [25]. The Parikh-Wilczek model regards the Hawking radiation as a tunneling process in some stationary vacuum.…”

Section: Nonthermal Correction Via Back Reactionmentioning

confidence: 99%

Nonthermal correction to black hole spectroscopy

Wen

2015

Eur. Phys. J. C

View full text Add to dashboard Cite

Area spectrum of black holes has been obtained via various methods such as quasinormal modes, adiabatic invariance and angular momentum. Among those methods, calculations were done by assuming black holes in thermal equilibrium. Nevertheless, black holes in the asymptotically flat space usually have a negative specific heat and therefore tend to stay away from thermal equilibrium. Even for black holes with a positive specific heat, the temperature may still not be well defined in the process of radiation, due to the back reaction of a decreasing mass. With respect to these facts, it is very likely that Hawking radiation is nonthermal and the area spectrum is no longer equidistant. In this note, we would like to illustrate how the area spectrum of black holes is corrected by this nonthermal effect. Area law and logarithmic correctionA finite size system often displays a discrete energy spectrum as regards quantum fluctuations. It was suggested that since the dynamics of a black hole is uniquely determined by its charge(s), which is closely related to the finite region enclosed by the horizon, one expects the mass or area spectrum to display a similar discreteness [1,2]. There were many proposals to obtain the area spectrum for various black holes since then. Earlier methods of quantizing the horizon area are mostly based on real or imaginary parts of the quasinormal modes [3][4][5][6][7][8][9][10][11][12]. Recently the application of an adiabatic invariant action variable did not use the quasinormal modes [13,14] and the idea of quantizing the angular momentum to obtain the area spectrum first appeared in the study of non-extremal RN black holes [15]. The various methods of quantization have settled on a spectrum of equidistant discreteness,a

show abstract

Section: Nonthermal Correction Via Back Reactionmentioning

confidence: 99%

Nonthermal correction to black hole spectroscopy

Wen

2015

Eur. Phys. J. C

View full text Add to dashboard Cite

show abstract

“…ω j , of the emitted field quanta. The probability for this radiation to occur is given by the following product of Γ's [17][18][19] which is defined in eq. (3.3)…”

Section: Jhep05(2014)074mentioning

confidence: 99%

“…This then provides a possible resolution of the information paradox when the specific conditions are imposed. The above arguments work even in the case where one ignores the quantum corrections [17][18][19], i.e. if one lets α 1 = 0.…”

Section: Jhep05(2014)074mentioning

confidence: 99%

Self-similarity, conservation of entropy/bits and the black hole information puzzle

Singleton

Vagenas

Zhu

2014

J. High Energ. Phys.

View full text Add to dashboard Cite

John Wheeler coined the phrase "it from bit" or "bit from it" in the 1980s. However, much of the interest in the connection between information, i.e. "bits", and physical objects, i.e. "its", stems from the discovery that black holes have characteristics of thermodynamic systems having entropies and temperatures. This insight led to the information loss problem -what happens to the "bits" when the black hole has evaporated away due to the energy loss from Hawking radiation? In this essay we speculate on a radical answer to this question using the assumption of self-similarity of quantum correction to the gravitational action and the requirement that the quantum corrected entropy be well behaved in the limit when the black hole mass goes to zero.

show abstract

“…Recently, such an idea has been employed by Chen and Shao [28]. They have modified the scenario of [26] by adding the quantum gravity effects.…”

mentioning

confidence: 99%

Entropy Conservation of Linear Dilaton Black Holes in Quantum Corrected Hawking Radiation

2011

View full text Add to dashboard Cite

It has been shown recently that information is lost in the Hawking radiation of the linear dilaton black holes in various theories when applying the tunneling formalism of Parikh and Wilczek without considering quantum gravity effects. In this paper, we recalculate the emission probability by taking into account the log-area correction to the Bekenstein-Hawking entropy and the statistical correlation between quanta emitted. The crucial role of the quantum gravity effects on the information leakage and black hole remnant is highlighted. The entropy conservation of the linear dilaton black holes is discussed in detail. We also model the remnant as an extreme linear dilaton black hole with a pointlike horizon in order to show that such a remnant cannot radiate and its temperature becomes zero. In summary, we show that the information can also leak out of the linear dilaton black holes together with preserving unitarity in quantum mechanics.

show abstract

Information loss and entropy conservation in quantum corrected Hawking radiation

Cited by 43 publications

References 52 publications

Nonthermal correction to black hole spectroscopy

Nonthermal correction to black hole spectroscopy

Self-similarity, conservation of entropy/bits and the black hole information puzzle

Entropy Conservation of Linear Dilaton Black Holes in Quantum Corrected Hawking Radiation

Contact Info

Product

Resources

About