Hawking radiation and strong gravity black holes

15th Marcel Grossmann Meeting, Rome, 2018, 2018

The author is considering 2 possible scenarios of Black Holes evaporation. First one coincide with well known S. Hawking's ( ,1975) ) scenarios, according to which actually Black Holes (created after the Big Bang, perhaps) with should evaporate, while another, which would take into account the occurency of Mass particles Bound states ([1]), especially Bose mass particles, of which the Higgs boson is of special interest. The second scenarios suppose a concurrence between the Hawking process and Bose mass particles exponentially fast accumulation with a rate of Black Hole's mass evolution. When the time is going to ∞ the mass of a Black Hole is going to 0. The time of diminishing by a half of the initial mass of a Black Hole is such, that it corresponds to ~ 54700 sec=15.19 hours for a Black Hole of mass nearly 1 mln tones in weight. This would occur due to generation of a Higgs boson (s=o) with mass m_Higgs=1Tev. If the Higgs boson mass is 125Gev, the time of diminishing by a half of the Black Hole's mass would be ~ 97 sec.

Journal of Cosmology and …, 2008

We study the properties of black holes of mass 10^4--10^{11} GeV in models with the fundamental scale of gravity at the TeV. These black holes could be produced in the collision of a ultrahigh energy cosmic ray with a dark matter particle in our galactic halo or with another cosmic ray. We show that QCD bremsstrahlung and pair production processes are unable to thermalize the particles exiting the black hole, so a chromosphere is never formed during Hawking evaporation. We evaluate with HERWIG the spectrum of stable 4-dim particles emitted during the Schwarzschild phase and find that in all cases it is peaked at energies around 0.2 GeV, with an approximate 43% of neutrinos, 28% of photons, 16% of electrons and 13% of protons. Bulk gravitons are peaked at higher energies, they account for a 0.4% of the particles (16% of the total energy) emitted by the most massive black holes in n=6 extra dimensions or just the 0.02% of the particles (1.4% of the energy) emitted by a 10 TeV black hole for n=2.

2018

The author is considering 2 possible scenarios of Black Holes evaporation. First one coincide with well known S. Hawking’s (1974,1975) scenarios, according to which actually Black Holes (created after the Big Bang, perhaps) with should evaporate, while another, which would take into account the occurency of Mass particles Bound states ([1]), especially Bose mass particles, of which the Higgs boson is of special interest. The second scenarios suppose a concurrence between the Hawking process and Bose mass particles exponentially fast accumulation with a rate of Black Hole’s mass evolution. When the time is going to ∞ the mass of a Black Hole is going to 0. The time of diminishing by a half of the initial mass of a Black Hole is such, that it corresponds to ~ 54700 sec=15.19 hours for a Black Hole of mass nearly 1 mln tones in weight. This would occur due to generation of a Higgs boson (s=o) with mass m_Higgs=1Tev. If the Higgs boson mass is 125Gev, the time of diminishing by a half o...

Review and "non quantum" analysis of Stephen Hawking's paper "Particle Creation by Black Holes" (1975), questioning his "Black Hole Evaporation" hypothesis. Supporting the analysis is the extremely broad range of scientific "difference of opinions" where theoretical Black Hole physics is concerned.

Classical and Quantum Gravity, 2005

A paradigm describing black hole evaporation in non-perturbative quantum gravity is developed by combining two sets of detailed results: i) resolution of the Schwarzschild singularity using quantum geometry methods [1, 2]; and ii) time-evolution of black holes in the trapping and dynamical horizon frameworks [3, 4, 5, 6]. Quantum geometry effects introduce a major modification in the traditional space-time diagram of black hole evaporation, providing a possible mechanism for recovery of information that is classically lost in the process of black hole formation. The paradigm is developed directly in the Lorentzian regime and necessary conditions for its viability are discussed. If these conditions are met, much of the tension between expectations based on space-time geometry and structure of quantum theory would be resolved.

Journal of High Energy Physics, 2015

In an earlier work, Kawai et al. proposed a model of black-hole formation and evaporation, in which the geometry of a collapsing shell of null dust is studied, including consistently the back reaction of its Hawking radiation. In this note, we illuminate the implications of their work, focusing on the resolution of the information loss paradox and the problem of the firewall.

1994

This thesis is a review of black hole evaporation with emphasis on recent results obtained for two dimensional black holes. First, the geometry of the most general stationary black hole in four dimensions is described and some classical quantities are dened. Then, a derivation of the spectrum of the radiation emitted during the evaporation is presented. In section four, a t w o dimensional model which has black hole solutions is introduced, the so-called CGHS model. These two dimensional black holes are found to evaporate. Unlike the four dimensional case, the evaporation process can be studied analytically as long as the mass of the black hole is well above the two dimensional analog of the Planck mass. Finally, some proposals for resolving the so-called information paradox are reviewed and it is concluded that none of them is fully satisfactory.

Physical Review D, 1997

Journal of High Energy Physics, 2018

The evaporation of black holes raises a number of conceptual issues, most of them related to the final stages of evaporation, where the interplay between the central singularity and Hawking radiation cannot be ignored. Regular models of black holes replace the central singularity with a nonsingular spacetime region, in which an effective classical geometric description is available. It has been argued that these models provide an effective, but complete, description of the evaporation of black holes at all times up to their eventual disappearance. However, here we point out that known models fail to be self-consistent: the regular core is exponentially unstable against perturbations with a finite timescale, while the evaporation time is infinite, therefore making the instability impossible to prevent. We also discuss how to overcome these difficulties, highlighting that this can be done only at the price of accepting that these models cannot be fully predictive regarding the final s...

A conjecture is made that the standard derivation of the black hole evaporation effect which uses infinite frequency wave modes is inadequate to describe black hole physics. The proposed resolution is that the problem is not due to the absence of the as yet unknown "correct" derivation but rather that the effect does not exist.