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General theory for thermal pulses of finite amplitude in nuclear shell-burnings

Journal Article:

Abstract

Theory for thermal pulses of nuclear shell-burning is advanced to include the case of finite amplitude. The aims are to predict the progress of thermal pulse quantitatively and to obtain the peak values of the temperature and nuclear energy generation rate without making detailed numerical computation of stellar structure. In order to attain them the physical processes involved in the progress of the pulse are clarified using the concepts of the flatness of the shell source, which destabilizes nuclear burning, and the effect of radiation pressure, which stabilizes it. It is shown that the progress of the pulse can be predicted quantitatively when the pressure and the gravitational potential of the burning shell are specified for the onset stage of the pulse. The pulse height is determined mainly by the initial pressure; the higher initial pressure results in the higher pulse. Mass dependence is also obtained by approximating the gravitational potential by that of white dwarfs. The initial pressure is the quantity which is determined in the course of evolution preceding the pulse. The theory is shown to give a satisfactory agreement with numerical computations for a wide variety of the preceding evolutions, i.e., both for the case of the  More>>
Authors:
Sugimoto, D; [1]  Fujimoto, M Y
  1. Tokyo Univ. (Japan). Coll. of General Education
Publication Date:
Sep 01, 1978
Product Type:
Journal Article
Reference Number:
AIX-10-475417; EDB-80-007373
Resource Relation:
Journal Name: Publ. Astron. Soc. Jpn.; (Japan); Journal Volume: 30:3
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; RED GIANT STARS; NUCLEAR REACTION KINETICS; STAR EVOLUTION; WHITE DWARF STARS; HELIUM; PRESSURE DEPENDENCE; PULSES; STAR MODELS; CRYOGENIC FLUIDS; DWARF STARS; ELEMENTS; FLUIDS; GIANT STARS; KINETICS; MATHEMATICAL MODELS; NONMETALS; RARE GASES; REACTION KINETICS; STARS; 640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources
OSTI ID:
5911509
Country of Origin:
Japan
Language:
English
Other Identifying Numbers:
Journal ID: CODEN: PASJA
Submitting Site:
INIS
Size:
Pages: 467-482
Announcement Date:

Journal Article:

Citation Formats

Sugimoto, D, and Fujimoto, M Y. General theory for thermal pulses of finite amplitude in nuclear shell-burnings. Japan: N. p., 1978. Web.
Sugimoto, D, & Fujimoto, M Y. General theory for thermal pulses of finite amplitude in nuclear shell-burnings. Japan.
Sugimoto, D, and Fujimoto, M Y. 1978. "General theory for thermal pulses of finite amplitude in nuclear shell-burnings." Japan.
@misc{etde_5911509,
title = {General theory for thermal pulses of finite amplitude in nuclear shell-burnings}
author = {Sugimoto, D, and Fujimoto, M Y}
abstractNote = {Theory for thermal pulses of nuclear shell-burning is advanced to include the case of finite amplitude. The aims are to predict the progress of thermal pulse quantitatively and to obtain the peak values of the temperature and nuclear energy generation rate without making detailed numerical computation of stellar structure. In order to attain them the physical processes involved in the progress of the pulse are clarified using the concepts of the flatness of the shell source, which destabilizes nuclear burning, and the effect of radiation pressure, which stabilizes it. It is shown that the progress of the pulse can be predicted quantitatively when the pressure and the gravitational potential of the burning shell are specified for the onset stage of the pulse. The pulse height is determined mainly by the initial pressure; the higher initial pressure results in the higher pulse. Mass dependence is also obtained by approximating the gravitational potential by that of white dwarfs. The initial pressure is the quantity which is determined in the course of evolution preceding the pulse. The theory is shown to give a satisfactory agreement with numerical computations for a wide variety of the preceding evolutions, i.e., both for the case of the core in red giant stars and of the accreting white dwarfs.}
journal = {Publ. Astron. Soc. Jpn.; (Japan)}
volume = {30:3}
journal type = {AC}
place = {Japan}
year = {1978}
month = {Sep}
}