Spacetime thermodynamics in the presence of torsion

TL;DR

This paper extends spacetime thermodynamics to Einstein-Cartan theory with torsion, deriving gravitational equations from horizon entropy and non-equilibrium thermodynamics, highlighting the role of torsion and horizon properties.

Contribution

It generalizes Jacobson's thermodynamic derivation of Einstein equations to include torsion in Einstein-Cartan theory, introducing non-equilibrium entropy production terms.

Findings

Derived Einstein-Cartan equations from horizon thermodynamics.

Established the notion of local causal horizons with torsion.

Highlighted the impact of torsion on black hole horizon properties.

Abstract

It was shown by Jacobson in 1995 that the Einstein equation can be derived as a local constitutive equation for an equilibrium spacetime thermodynamics. With the aim to understand if such thermodynamical description is an intrinsic property of gravitation, many attempts have been done so far to generalise this treatment to a broader class of gravitational theories. Here we consider the case of the Einstein-Cartan theory as a prototype of theories with non-propagating torsion. In doing so, we study the properties of Killing horizons in the presence of torsion, establish the notion of local causal horizon in Riemann-Cartan spacetimes, and derive the generalised Raychaudhuri equation for this kind of geometries. Then, starting with the entropy that can be associated to these local causal horizons, we derive the Einstein-Cartan equation by implementing the Clausius equation. We outline two ways of proceeding with the derivation depending on whether we take torsion as a geometric field or as a matter field. In both cases we need to add internal entropy production terms to the Clausius equation as the shear and twist cannot be taken to be zero a priori for our setup. This fact implies the necessity of a non-equilibrium thermodynamics treatment for the local causal horizon. Furthermore, it implies that a non-zero twist at the horizon will in general contribute to the Hartle-Hawking tidal heating for black holes with possible implications for future observations.