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Gravothermal catastrophe of finite amplitude

Abstract

Development of the gravothermal catastrophe is followed numerically for self-gravitating gas system enclosed by an adiabatic wall, which is isothermal in the initial state. It is found that the final fate of the catastrophe is in two ways depending on the initial perturbations. When the initial perturbation produces a temperature distribution decreasing outward, the contraction proceeds in the central region and the central density increases unlimitedly, as the heat flows outward. When the initial temperature distribution is increasing outward, on the other hand, the central region expands as the heat flows into the central region. Then the density contrast is reduced and finally the system reaches another isothermal configuration with the same energy but with a lower density contrast and a higher entropy. This final configuration is gravothermally stable and may be called a thermal system. In the former case of the unlimited contraction, the final density profile is determined essentially by the density and temperature dependence of the heat conductivity. In the case of a system under the force of the inverse square law, the final density distribution is well approximated by a power law so that the mass contained in the condensed core is relatively small. A possibility  More>>
Authors:
Hachisu, I; Sugimoto, D; [1]  Nakada, Y; Nomoto, K
  1. Tokyo Univ. (Japan). Coll. of General Education
Publication Date:
Aug 01, 1978
Product Type:
Journal Article
Reference Number:
AIX-10-471830; EDB-79-133590
Resource Relation:
Journal Name: Prog. Theor. Phys. (Kyoto); (Japan); Journal Volume: 60:2
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; COSMIC GASES; GRAVITATIONAL COLLAPSE; BLACK HOLES; ENTROPY; GALAXIES; GRAVITATIONAL FIELDS; PLASMA DENSITY; STABILITY; STARS; THERMAL CONDUCTIVITY; THERMAL EQUILIBRIUM; EQUILIBRIUM; FLUIDS; GASES; PHYSICAL PROPERTIES; THERMODYNAMIC PROPERTIES; 640105* - Astrophysics & Cosmology- Galaxies
OSTI ID:
5905507
Country of Origin:
Japan
Language:
English
Other Identifying Numbers:
Journal ID: CODEN: PTPKA
Submitting Site:
INIS
Size:
Pages: 393-402
Announcement Date:

Citation Formats

Hachisu, I, Sugimoto, D, Nakada, Y, and Nomoto, K. Gravothermal catastrophe of finite amplitude. Japan: N. p., 1978. Web. doi:10.1143/PTP.60.393.
Hachisu, I, Sugimoto, D, Nakada, Y, & Nomoto, K. Gravothermal catastrophe of finite amplitude. Japan. doi:10.1143/PTP.60.393.
Hachisu, I, Sugimoto, D, Nakada, Y, and Nomoto, K. 1978. "Gravothermal catastrophe of finite amplitude." Japan. doi:10.1143/PTP.60.393. https://www.osti.gov/servlets/purl/10.1143/PTP.60.393.
@misc{etde_5905507,
title = {Gravothermal catastrophe of finite amplitude}
author = {Hachisu, I, Sugimoto, D, Nakada, Y, and Nomoto, K}
abstractNote = {Development of the gravothermal catastrophe is followed numerically for self-gravitating gas system enclosed by an adiabatic wall, which is isothermal in the initial state. It is found that the final fate of the catastrophe is in two ways depending on the initial perturbations. When the initial perturbation produces a temperature distribution decreasing outward, the contraction proceeds in the central region and the central density increases unlimitedly, as the heat flows outward. When the initial temperature distribution is increasing outward, on the other hand, the central region expands as the heat flows into the central region. Then the density contrast is reduced and finally the system reaches another isothermal configuration with the same energy but with a lower density contrast and a higher entropy. This final configuration is gravothermally stable and may be called a thermal system. In the former case of the unlimited contraction, the final density profile is determined essentially by the density and temperature dependence of the heat conductivity. In the case of a system under the force of the inverse square law, the final density distribution is well approximated by a power law so that the mass contained in the condensed core is relatively small. A possibility of formation of a black hole in stellar systems is also discussed.}
doi = {10.1143/PTP.60.393}
journal = {Prog. Theor. Phys. (Kyoto); (Japan)}
volume = {60:2}
journal type = {AC}
place = {Japan}
year = {1978}
month = {Aug}
}