Numerical thermodynamic studies of classical gravitational collapse in 3+1 and 4+1 dimensions

Details Numerical thermodynamic studies of classical gravitational collapse in 3+1 and 4+1 dimensions Numerical thermodynamic studies of classical gravitational collapse in 3+1 and 4+1 dimensions

2011-03-28

arxiv.org/abs/1103.5272v2

Phys. Rev. D. 84, 084032 (2011)

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

35 pages, 14 figures, to appear in Phys. Rev. D

Scientific paper

10.1103/PhysRevD.84.084032

We study a thermodynamic potential during the classical gravitational collapse of a 4D (3+1) massless scalar field to a Schwarzschild black hole in isotropic coordinates. We track numerically the function $F(t)=-dI/dt=-L$, where $I$ is the total action of matter plus gravitation, $L$ the total Lagrangian and $t$ is the time measured by a stationary clock at infinity. At late stages in the collapse, this function can be identified with the free energy $F=E-TS$ of the black hole where $E$ is the ADM mass, $T$ the Hawking temperature and $S$ the entropy. From standard black hole thermodynamics, the free energy of a 4D Schwarzschild black hole is equal to $E/2$. Our numerical simulations show that at late stages of the collapse the function $-L$ approaches a constant to within 5% of the value of $E/2$. We also present numerical results for the thermodynamics of 5D collapse where the free energy in this case is $E/3$. In both 4D and 5D, our numerical simulations show that at late stages of the collapse, the metric fields are nonstationary in a thin region just behind the event horizon (and are basically static everywhere else). The entropy stems mostly from the nonstationary interior region where there is a significant dip (negative contribution) to the free energy.

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