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Title:
Models for Type I supernova. I - Detonations in white dwarfs
Authors:
Woosley, S. E.; Taam, R. E.; Weaver, T. A.
Affiliation:
AA(Lick Observatory, Santa Cruz; California, University, Livermore), AB(Northwestern University, Evanston, IL), AC(California, University, Livermore)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 301, Feb. 15, 1986, p. 601-623. (ApJ Homepage)
Publication Date:
02/1986
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
BINARY STARS, NUCLEAR FUSION, STELLAR EVOLUTION, STELLAR PHYSICS, SUPERNOVAE, WHITE DWARF STARS, DENSITY DISTRIBUTION, DETONATION, HYDRODYNAMICS, LIGHT CURVE, STELLAR ENVELOPES, STELLAR GRAVITATION, STELLAR LUMINOSITY, STELLAR MASS ACCRETION, STELLAR MODELS, STELLAR OSCILLATIONS
DOI:
10.1086/163926
Bibliographic Code:
1986ApJ...301..601W

Abstract

In a series of papers, the properties of white dwarfs provoked into nuclear instability by accretion will be explored. The results bear many close similarities to the observed properties of Type I supernovae, especially their energetics, light curves, nucleosynthesis, and spectra. In this paper a class of "detonating white dwarfs" is explored. The final evolution of carbon-oxygen white dwarfs in binary systems undergoing mass exchange at rates in the range 10-9 to 10-8M_sun;yr-1 is considered. Three models are constructed having initial carbon-oxygen core masses 0.5, 0.8, and 1.2 M_sun; and accreting helium at rates of 10-8, 2×10-9, and 10-9M_sun;yr-1, respectively. In all cases continued evolution leads to the accumulation of a thick helium layer surrounding the core, degenerate helium ignition, detonation and mass ejection. Detailed isotopic nucleosynthesis has also been computed for these models and implications for Galactic chemical evolution and gamma-line astronomy are discussed. At present, the class of detonating models does not agree well with spectroscopic constraints upon common Type I events.

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