Black hole evaporation and semiclassicality at large D
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Black hole evaporation and semiclassicality at large D. / Holdt-Sørensen, Frederik; McGady, David A.; Wintergerst, Nico.
I: Physical Review D, Bind 102, Nr. 2, 026016, 15.07.2020.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Black hole evaporation and semiclassicality at large D
AU - Holdt-Sørensen, Frederik
AU - McGady, David A.
AU - Wintergerst, Nico
PY - 2020/7/15
Y1 - 2020/7/15
N2 - Black holes of sufficiently large initial radius are expected to be well described by a semiclassical analysis at least until half of their initial mass has evaporated away. For a small number of spacetime dimensions, this holds as long as the black hole is parametrically larger than the Planck length. In that case, curvatures are small, and backreaction onto geometry is expected to be well described by a time-dependent classical metric. We point out that at large D, small curvature is insufficient to guarantee a valid semiclassical description of black holes. Instead, the strongest bounds come from demanding that the rate of change of the geometry is small and that black holes scramble information faster than they evaporate. This is a consequence of the enormous power of Hawking radiation in D dimensions due to the large available phase space and the resulting minuscule evaporation times. Asymptotically, only black holes with entropies S >= DD+3 ogD are semiclassical. We comment on implications for realistic quantum gravity models in D
AB - Black holes of sufficiently large initial radius are expected to be well described by a semiclassical analysis at least until half of their initial mass has evaporated away. For a small number of spacetime dimensions, this holds as long as the black hole is parametrically larger than the Planck length. In that case, curvatures are small, and backreaction onto geometry is expected to be well described by a time-dependent classical metric. We point out that at large D, small curvature is insufficient to guarantee a valid semiclassical description of black holes. Instead, the strongest bounds come from demanding that the rate of change of the geometry is small and that black holes scramble information faster than they evaporate. This is a consequence of the enormous power of Hawking radiation in D dimensions due to the large available phase space and the resulting minuscule evaporation times. Asymptotically, only black holes with entropies S >= DD+3 ogD are semiclassical. We comment on implications for realistic quantum gravity models in D
KW - ENTROPY
KW - GRAVITY
U2 - 10.1103/PhysRevD.102.026016
DO - 10.1103/PhysRevD.102.026016
M3 - Journal article
VL - 102
JO - Physical Review D
JF - Physical Review D
SN - 2470-0010
IS - 2
M1 - 026016
ER -
ID: 245666476