Heat flow in the postquasistatic approximation

Details Heat flow in the postquasistatic approximation Heat flow in the postquasistatic approximation

2010-05-10

arxiv.org/abs/1005.1637v2

Phys. Rev. D 82, 044003 (2010)

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

5 pages, 5 figures

Scientific paper

10.1103/PhysRevD.82.044003

We apply the postquasistatic approximation to study the evolution of spherically symmetric fluid distributions undergoing dissipation in the form of radial heat flow. For a model which corresponds to an incompressible fluid departing from the static equilibrium, it is not possible to go far from the initial state after the emission of a small amount of energy. Initially collapsing distributions of matter are not permitted. Emission of energy can be considered as a mechanism to avoid the collapse. If the distribution collapses initially and emits one hundredth of the initial mass only the outermost layers evolve. For a model which corresponds to a highly compressed Fermi gas, only the outermost shell can evolve with a shorter hydrodynamic time scale.

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