Fate of gravitational collapse in semiclassical gravity

By C. Barceló, Stefano Liberati, S. Sonego, Matt Visser. 2007

176 citations recorded by the source corpus.

While the outcome of gravitational collapse in classical general relativity is unquestionably a black hole, up to now no full and complete semiclassical description of black hole formation has been thoroughly investigated. Here we revisit the standard scenario for this process. By analyzing how semiclassical collapse proceeds we show that the very formation of a trapping horizon can be seriously questioned for a large set of, possibly realistic, scenarios. We emphasize that in principle the theoretical framework of semiclassical gravity certainly allows the formation of trapping horizons. What we are questioning here is the more subtle point of whether or not the standard black hole picture is appropriate for describing the end point of realistic collapse. Indeed if semiclassical physics were in some cases to prevent formation of the trapping horizon, then this suggests the possibility of new collapsed objects which can be much less problematic, making it unnecessary to confront the information paradox or the runaway end point problem.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a6e23e8ddb04ff37ef970957b57bf45ec63761fd

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Citations in the corpus

TESTING THE NO-HAIR THEOREM WITH OBSERVATIONS IN THE ELECTROMAGNETIC SPECTRUM. II. BLACK HOLE IMAGES (2010, background): “…been suggested, which include naked singularities (Manko & Novikov 1992), exotic stellar objects (Friedberg, Lee, & Pang 1987; Mazur & Mottola 2001; Barceló et al. 2008), as well as a breakdown of general relativity itself on horizon scales (e.g., Yunes & Pretorius 2009; c.f. Psaltis et al. 2008).”
Stellar structure models in modified theories of gravity: Lessons and challenges (2019, background): “Such corrections might significantly raise the central density of the star, potentially allowing new classes of relativistic stars not present in GR, such as black stars [354], though explicit models are yet to be explored.”
Tests for the existence of black holes through gravitational wave echoes (2017, background): “Some of these models – including also black stars [22, 23], superspinars [24] or collapsed polymers [25, 26] – predict that large quantum backreaction should affect the horizon geometry even for macroscopic objects.”
Phenomenological aspects of black holes beyond general relativity (2018, background): “[57] Carlos Barceló, Stefano Liberati, Sebastiano Sonego, and Matt Visser, “Fate of gravitational collapse in semiclassical gravity,” Phys.”
Black holes in general relativity (2009, background): “(See the accompanying article [55], and reference [46], for more details on the specific proposal by the current author and his collaborators.”
Time Dependence of Hawking Radiation Entropy (2013, background): “Interest in black hole information [1, 2, 3, 4, 5, 6, 7, 8, 9, 10, 11, 12, 13, 14, 15, 16, 17, 18, 19, 20, 21, 22, 23, 24, 25, 26, 27, 28, 29, 30, 31, 32, 33, 34, 35, 36, 37, 38, 39, 40, 41, 42, 43, 44, 45, 46, 47, 48, 49, 50, 51, 52, 53, 54, 55, 56, 57, 58, 59, 60, 61, 62, 63, 64, 65, 66, 67, 68, 6”