Rindler horizon entropy from nonstationarity

Abstract

Finite entropy and energy are obtained for the horizon of a Rindler observer on the grounds of the nonstatic character of the geometry beyond the horizon. Edery - Constantineau prescription is used to find the dynamical phase space of this particular spacetime. The number of microstates rooted from the ignorance of a Rindler observer of the parameter $t$ from the nonstationary region is calculated. We suggest that the gravitational energy density constructed by means of the horizon energy and using the Holographic Principle is proportional to $g^2$, similar with a result recently obtained by Padmanabhan and with the energy density of the electromagnetic field.

8 pages, no figures, version published in PLB 703(5),(2011) pp. 641-644, DOI: 10.1016/j.physletb.2011.08.068

References in corpus (5)

• Tunnelling, Temperature and Taub-NUT Black Holes
• Interior of a Schwarzschild black hole revisited
• The radiation of a uniformly accelerated charge is beyond the horizon: a simple derivation
• Is the Rindler horizon energy nonvanishing ?
• On The Black Hole Interior Spacetime

Cited by in corpus (4)

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• Role of the remnant symmetries in gravitational theories based on absolute parallelism: a 2D standpoint