Heat flow in the postquasistatic approximation

被引：2

作者：

Rodriguez-Mueller, B. ^{[1
]}

Peralta, C. ^{[2
,3
]}

Barreto, W.

Rosales, L. ^{[4
]}

机构：

[1] San Diego State Univ, Coll Sci, Computat Sci Res Ctr, San Diego, CA 92182 USA

[2] Deutsch Wetterdienst, D-63067 Offenbach, Germany

[3] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia

[4] Univ Expt Politecn Antonio Jose de Sucre, Lab Fis Computac, Puerto Ordaz, Venezuela

来源：

PHYSICAL REVIEW D | 2010年 / 82卷 / 04期

关键词：

RADIATING FLUID SPHERES; GRAVITATIONAL COLLAPSE; EVOLUTION;

D O I：

10.1103/PhysRevD.82.044003

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 that 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 that corresponds to a highly compressed Fermi gas, only the outermost shell can evolve with a shorter hydrodynamic time scale.

引用

页数：5

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