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Title: Time evolution of entropy in gravitational collapse

Abstract

We study the time evolution of the entropy of a collapsing spherical domain wall, from the point of view of an asymptotic observer, by investigating the entropy of the entire system (i.e. domain wall and radiation) and induced radiation alone during the collapse. By taking the difference, we find the entropy of the collapsing domain wall, since this is the object which will form a black hole. We find that for large values of time (times larger than t/R{sub s} ≈ 8), the entropy of the collapsing domain wall is a constant, which is of the same order as the Bekenstein-Hawking entropy.

Authors:
 [1]
  1. HEPCOS, Department of Physics, SUNY at Buffalo, Buffalo, NY 14260-1500 (United States)
Publication Date:
OSTI Identifier:
22273161
Resource Type:
Journal Article
Journal Name:
Journal of Cosmology and Astroparticle Physics
Additional Journal Information:
Journal Volume: 2009; Journal Issue: 06; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 1475-7516
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTROPHYSICS; ASYMPTOTIC SOLUTIONS; BLACK HOLES; COSMOLOGY; ENTROPY; EVOLUTION; GRAVITATIONAL COLLAPSE; TIME DEPENDENCE

Citation Formats

Greenwood, Eric. Time evolution of entropy in gravitational collapse. United States: N. p., 2009. Web. doi:10.1088/1475-7516/2009/06/032.
Greenwood, Eric. Time evolution of entropy in gravitational collapse. United States. https://doi.org/10.1088/1475-7516/2009/06/032
Greenwood, Eric. 2009. "Time evolution of entropy in gravitational collapse". United States. https://doi.org/10.1088/1475-7516/2009/06/032.
@article{osti_22273161,
title = {Time evolution of entropy in gravitational collapse},
author = {Greenwood, Eric},
abstractNote = {We study the time evolution of the entropy of a collapsing spherical domain wall, from the point of view of an asymptotic observer, by investigating the entropy of the entire system (i.e. domain wall and radiation) and induced radiation alone during the collapse. By taking the difference, we find the entropy of the collapsing domain wall, since this is the object which will form a black hole. We find that for large values of time (times larger than t/R{sub s} ≈ 8), the entropy of the collapsing domain wall is a constant, which is of the same order as the Bekenstein-Hawking entropy.},
doi = {10.1088/1475-7516/2009/06/032},
url = {https://www.osti.gov/biblio/22273161}, journal = {Journal of Cosmology and Astroparticle Physics},
issn = {1475-7516},
number = 06,
volume = 2009,
place = {United States},
year = {Mon Jun 01 00:00:00 EDT 2009},
month = {Mon Jun 01 00:00:00 EDT 2009}
}