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Thermodynamics of scalar-tensor gravity
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abstract
Previously, the Einstein equation has been described as an equation of state, general relativity as the equilibrium state of gravity, and $f({\cal R})$ gravity as a non-equilibrium one. We apply Eckart's first order thermodynamics to the effective dissipative fluid describing scalar-tensor gravity. Surprisingly, we obtain simple expressions for the effective heat flux, "temperature of gravity", shear and bulk viscosity, and entropy density, plus a generalized Fourier law in a consistent Eckart thermodynamical picture. Well-defined notions of temperature and approach to equilibrium, missing in the current thermodynamics of spacetime scenarios, naturally emerge.
Forward citations
Cited by 3 Pith papers
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Gravitational Waves as Thermodynamic Shear Excitations in Scalar-Tensor Gravity
In scalar-tensor gravity, a transverse-traceless gravitational wave performs gauge-invariant shear work on the scalar-field fluid, with power = (KT/4) times the squared strain rate.
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Towards a causal effective thermodynamics of scalar-tensor gravity
Extends scalar-tensor gravity thermodynamics to causal Israel-Stewart model via timelike heat flux ansatz, decoupling T and K while preserving GR equilibrium.
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Black hole interiors in the thermal view of scalar-tensor gravity
In the thermal view of Brans-Dicke gravity, black hole singularities are 'hot': the effective temperature KT diverges as 1/t, and a fluid with P=wρ controls whether gravity approaches or departs from general relativity.
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