Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (204) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
The evolution of massive stars including mass loss - Presupernova models and explosion
Authors:
Woosley, S. E.; Langer, Norbert; Weaver, Thomas A.
Affiliation:
AA(Lick Observatory, Santa Cruz; Lawrence Livermore National Lab., Livermore, CA), AB(Göttingen, Univ.-Sternwarte, Germany; Lick Observatory, Santa Cruz, CA), AC(Lawrence Livermore National Lab., Livermore, CA)
Publication:
Astrophysical Journal - Part 1 (ISSN 0004-637X), vol. 411, no. 2, p. 823-839. (ApJ Homepage)
Publication Date:
07/1993
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
ASTRONOMICAL MODELS, MASSIVE STARS, NUCLEAR EXPLOSION EFFECT, STELLAR EVOLUTION, STELLAR MASS EJECTION, SUPERNOVAE, GRAVITATIONAL COLLAPSE, LIGHT CURVE, NUCLEAR FUSION, STELLAR INTERIORS, WOLF-RAYET STARS
DOI:
10.1086/172886
Bibliographic Code:
1993ApJ...411..823W

Abstract

The evolution of massive stars of 35, 40, 60, and 85 solar masses is followed through all stages of nuclear burning to the point of Fe core collapse. Critical nuclear reaction and mass-loss rates are varied. Efficient mass loss during the Wolf-Rayet (WR) stage is likely to lead to final masses as small as 4 solar masses. For a reasonable parameterization of the mass loss, there may be convergence of all WR stars, both single and in binaries, to a narrow band of small final masses. Our representative model, a 4.25 solar-mass WR presupernova derived from a 60 solar mass star, is followed through a simulated explosion, and its explosive nucleosynthesis and light curve are determined. Its properties are similar to those observed in Type Ib supernovae. The effects of the initial mass and mass loss on the presupernova structure of small mass WR models is also explored. Important properties of the presupernova star and its explosion can only be obtained by following the complete evolution starting on the main sequence.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints