Mass inflation in the loop black hole

The internal structure of a charged spherical black hole is still a topic of debate. In a non-rotating but aspherical gravitational collapse to form a spherical charged black hole, the backscattered gravitational wave tails enter the black hole and are blueshifted at the Cauchy horizon. This has a catastrophic effect if combined with an outflux crossing the Cauchy horizon: a singularity develops at the Cauchy horizon and the effective mass inflates. Recently, a numerical study of a massless scalar field in the Reissner-Nordström background suggested that a spacelike singularity may form before the Cauchy horizon forms. We will show that there exists an approximate analytic solution of the scalar-field equations which allows the mass-inflation singularity at the Cauchy horizon to exist. In particular, we see no evidence that the Cauchy horizon is preceded by a spacelike singularity.

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Mass inflation in a rotating charged black hole

Physical Review D ◽

10.1103/physrevd.53.7373 ◽

1996 ◽

Vol 53 (12) ◽

pp. 7373-7376 ◽

Cited By ~ 11

Author(s):

Alfio Bonanno

Keyword(s):

Black Hole ◽

Charged Black Hole ◽

Mass Inflation

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Inner structure of a charged black hole: An exact mass-inflation solution

Physical Review Letters ◽

10.1103/physrevlett.67.789 ◽

1991 ◽

Vol 67 (7) ◽

pp. 789-792 ◽

Cited By ~ 195

Author(s):

Amos Ori

Keyword(s):

Black Hole ◽

Charged Black Hole ◽

Exact Mass ◽

Mass Inflation

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Remarks on non-singular black holes

EPJ Web of Conferences ◽

10.1051/epjconf/201816801001 ◽

2018 ◽

Vol 168 ◽

pp. 01001 ◽

Cited By ~ 4

Author(s):

Valeri P. Frolov

Keyword(s):

Black Holes ◽

Black Hole ◽

Apparent Horizon ◽

External Observer ◽

Quantum Radiation ◽

Black Hole Background ◽

Black Hole Interior ◽

Mass Inflation ◽

The Given ◽

Self Consistency

We briefly discuss non-singular black hole models, with the main focus on the properties of non-singular evaporating black holes. Such black holes possess an apparent horizon, however the event horizon may be absent. In such a case, the information from the black hole interior may reach the external observer after the complete evaporation of the black hole. This model might be used for the resolution of the information loss puzzle. However, as we demonstrate, in a general case the quantum radiation emitted from the black hole interior, calculated in the given black hole background, is very large. This outburst of the radiation is exponentially large for models with the redshift function α = 1. We show that it can be suppressed by including a non-trivial redshift function. However, even this suppression is not enough to guarantee self-consistency of the model. This problem is a manifestation of a general problem, known as the "mass inflation". We briefly comment on possible ways to overcome this problem in the models of non-singular evaporating black holes.

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