Semiclassical Corrections to the Bekenstein-Hawking entropy of the BTZ Black Hole via Self-Gravitation

Abstract

Hawking radiation is viewed as a tunnelling process. In this way the effect of self-gravitation gives rise to semiclassical corrections to the entropy of the (2+1) BTZ black hole. The modified entropy, due to specific modelling of the self-gravitation effect, of the (2+1) BTZ black hole is evaluated. To first order in $\omega$ which is a shell of energy radiated outwards the event horizon of the BTZ black hole, modified entropy is proportional to the horizon. In this semiclassical analysis, corrections to the Bekenstein-Hawking formula $S_{BH}={\mathcal{A}}_H/4l_P^2$ are found to be negative and the proportionality factor connecting the modified entropy, $S_{bh}$, of the (2+1) BTZ black hole to the Bekenstein-Hawking entropy, $S_{BH}$, is evaluated to first order in $\omega$.

LaTeX, 8 pages, no figures, v3: minor typos corrected, v4: version to appear in Phys. Lett. B

References in corpus (2)

• Are Extremal 2D Black Holes Really Frozen ?
• Radiation via Tunneling in the Charged BTZ Black Hole

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