Hawking radiation power equations for black holes

Mistry, Ravi; Upadhyay, Sudhaker; Ali, Ahmed Farag; Faizal, Mir

doi:10.1016/j.nuclphysb.2017.08.010

Cited by 11 publications

(7 citation statements)

References 23 publications

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“…The equation was derived assuming the screen is placed close to the horizon, but respecting the radial NEC does not allow this. This should not be a particularly big issue since, up to an order one pre-factor, the evaporation rate should go as dM/dt ∼ β −2[31]. Which is consistent with Pennington's results[17] as well as ours.…”

supporting

confidence: 92%

Extracting Hawking radiation near the horizon of AdS black holes

Saraswat

Afshordi

2021

J. High Energ. Phys.

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We study how the evaporation rate of spherically symmetric black holes is affected through the extraction of radiation close to the horizon. We adopt a model of extraction that involves a perfectly absorptive screen placed close to the horizon and show that the evaporation rate can be changed depending on how close to the horizon the screen is placed. We apply our results to show that the scrambling time defined by the Hayden-Preskill decoding criterion, which is derived in Pennington’s work (arXiv:1905.08255) through entanglement wedge reconstruction is modified. The modifications appear as logarithmic corrections to Pennington’s time scale which depend on where the absorptive screen is placed. By fixing the proper distance between the horizon and screen we show that for small AdS black holes the leading order term in the scrambling time is consistent with Pennington’s scrambling time. However, for large AdS black holes the leading order Log contains the Bekenstein-Hawking entropy of a cell of characteristic length equal to the AdS radius rather than the entropy of the full horizon. Furthermore, using the correspondence between the radial null energy condition (NEC) and the holographic c-theorem, we argue that the screen cannot be arbitrarily close to the horizon. This leads to a holographic argument that black hole mining using a screen cannot significantly alter the lifetime of a black hole.

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confidence: 92%

Extracting Hawking radiation near the horizon of AdS black holes

Saraswat

Afshordi

2021

J. High Energ. Phys.

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“…Since, v<c, hence and so on (8) Hence, it is clear that the terms of higher power of v/c in equation (7) can be neglected and finally, we have…”

Section: Theoretical Discussionmentioning

confidence: 98%

“…Brajesh et al converted the Stephen-Boltzmann-Schwarzschild-Hawking radiation formula in terms of Chandrasekhar limit [M ch ] and calculated their values for different test black holes existing in XRBs and AGN [7]. Mistry et al gave a model for the Hawking radiation power for black holes in asymptotically flat, asymptotically Anti-de Sitter (AdS) and asymptotically de Sitter (dS) black holes which showed that at low frequency, this model for asymptotically flat black holes, corresponding to grey body factor depends on both the Hawking temperature as well as event horizon and also the same for both Schwarzschild AdS and Reissner-Nordström AdS solutions and only depends on the Hawking temperature at asymptotic frequency [8].…”

Section: Introductionmentioning

confidence: 99%

Relativistic Radiation Power of Spinning Black Holes

Mahto¹

2020

Int J Phys Stud Res

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In the present research paper, we have proposed a model for the relativistic radiation power using the Stephen-Boltzmann-Schwarzschild-Hawking radiation formula with the application of the variation of mass with velocity. We have concluded that the relativistic radiation power of spinning black hole decreases with the increase of the velocity and the mass of black hole is not only the function of radiation power of the spinning black holes, but also spinning velocity.

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“…A blackbody that emits radiant energy and has same relative spectral energy distribution at the same temperature, the difference in the energy distributions in smaller amount, is called greybody factor. Mistry et al [49] have obtained the Hawking radiation power equations in the background of asymptotically flat, AdS and dS BHs in (d + 1) dimensions by using the greybody factors for these BHs.…”

Section: Kdsmentioning

confidence: 99%

Effect of the magnetic charge on weak deflection angle and greybody bound of the black hole in Einstein-Gauss-Bonnet gravity

Javed,

Aqib,

Övgün

2022

Preprint

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The objective of this paper is to analyze the weak deflection angle of Einstein-Gauss-Bonnet gravity in the presence of plasma medium. To attain our results, we implement the Gibbons and Werner approach and use the Gauss-Bonnet theorem to Einstein gravity to acquire the resulting deflection angle of photon's ray in the weak field limit. Moreover, we illustrate the behavior of plasma medium and non-plasma mediums on the deflection of photon's ray in the framework of Einstein-Gauss-Bonnet gravity. Similarly, we observe the graphical influences of deflection angle on Einstein-Gauss-Bonnet gravity with the consideration of both plasma and non-plasma mediums. Later, we observe the rigorous bounds phenomenon of the greybody factor in contact with Einstein-Gauss-Bonnet gravity and calculate the outcomes, analyze graphically for specific values of parameters.

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Hawking radiation power equations for black holes

Cited by 11 publications

References 23 publications

Extracting Hawking radiation near the horizon of AdS black holes

Extracting Hawking radiation near the horizon of AdS black holes

Relativistic Radiation Power of Spinning Black Holes

Effect of the magnetic charge on weak deflection angle and greybody bound of the black hole in Einstein-Gauss-Bonnet gravity

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