Back reaction effects in black hole spacetimes

We solve the semiclassical Einstein equations for the static spherically symmetric case. Using expressions for the renormalized 〈Tμv〉, we study the effects of the back reaction on black hole spacetimes at the one-loop level. Two different situtaions appear depending on the graviton-matter balance. I...

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Publicado: 1988
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03702693_v212_n4_p411_Lousto
http://hdl.handle.net/20.500.12110/paper_03702693_v212_n4_p411_Lousto
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_03702693_v212_n4_p411_Lousto
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spelling paper:paper_03702693_v212_n4_p411_Lousto2023-06-08T15:36:30Z Back reaction effects in black hole spacetimes We solve the semiclassical Einstein equations for the static spherically symmetric case. Using expressions for the renormalized 〈Tμv〉, we study the effects of the back reaction on black hole spacetimes at the one-loop level. Two different situtaions appear depending on the graviton-matter balance. If matter is relevant, the temperature is increased and thus the lifetime decreased from their standard values TH= 1 8πMand τH=CM3. If the graviton is dominant T is smaller than TH and more important, it can have a maximum at M≈Mp and then go to zero. The connection with string theory is discussed. © 1988. 1988 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03702693_v212_n4_p411_Lousto http://hdl.handle.net/20.500.12110/paper_03702693_v212_n4_p411_Lousto
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
description We solve the semiclassical Einstein equations for the static spherically symmetric case. Using expressions for the renormalized 〈Tμv〉, we study the effects of the back reaction on black hole spacetimes at the one-loop level. Two different situtaions appear depending on the graviton-matter balance. If matter is relevant, the temperature is increased and thus the lifetime decreased from their standard values TH= 1 8πMand τH=CM3. If the graviton is dominant T is smaller than TH and more important, it can have a maximum at M≈Mp and then go to zero. The connection with string theory is discussed. © 1988.
title Back reaction effects in black hole spacetimes
spellingShingle Back reaction effects in black hole spacetimes
title_short Back reaction effects in black hole spacetimes
title_full Back reaction effects in black hole spacetimes
title_fullStr Back reaction effects in black hole spacetimes
title_full_unstemmed Back reaction effects in black hole spacetimes
title_sort back reaction effects in black hole spacetimes
publishDate 1988
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03702693_v212_n4_p411_Lousto
http://hdl.handle.net/20.500.12110/paper_03702693_v212_n4_p411_Lousto
_version_ 1768542084554293248

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