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PreprintCC BY 4.0arXiv

A Quasi-local Entropy for Black Hole Space-times

Abstract

We show that for static & spherically symmetric black hole geometries, the angular components of the Brown-York tensor on a finite radius boundary can be interpreted as the product of the Tolman-Ehrenfest temperature and a quasi-local entropy. This entropy vanishes at spatial infinity and monotonically increases as radius decreases, taking its maximum value on the horizon where it is equal to the Bekenstein-Hawking entropy. Thus, the behaviour of this entropy provides explicit verification of the covariant entropy conjecture.

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BibTeX
@misc{isichei2026quasilocal,
  title = {{A Quasi-local Entropy for Black Hole Space-times}},
  author = {Raymond Isichei},
  howpublished = {arXiv},
  year = {2026},
  month = aug,
  doi = {10.48550/arxiv.2608.28755},
  eprint = {2608.28755},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2608.28755},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - A Quasi-local Entropy for Black Hole Space-times
AU  - Raymond Isichei
PY  - 2026
DA  - 2026/08/28
PB  - arXiv
DO  - 10.48550/arxiv.2608.28755
UR  - https://arxiv.org/abs/2608.28755
AB  - We show that for static & spherically symmetric black hole geometries, the angular components of the Brown-York tensor on a finite radius boundary can be interpreted as the product of the Tolman-Ehrenfest temperature and a quasi-local entropy. This entropy vanishes at spatial infinity and monotonically increases as radius decreases, taking its maximum value on the horizon where it is equal to the Bekenstein-Hawking entropy. Thus, the behaviour of this entropy provides explicit verification of the covariant entropy conjecture.
ER  -