White dwarf models of supernovae and cataclysmic variables
If the accreting white dwarf increases its mass to the Chandrasekhar mass, it will either explode as a Type I supernova or collapse to form a neutron star. In fact, there is a good agreement between the exploding white dwarf model for Type I supernovae and observations. We describe various types of evolution of accreting white dwarfs as a function of binary parameters (i.e,. composition, mass, and age of the white dwarf, its companion star, and mass accretion rate), and discuss the conditions for the precursors of exploding or collapsing white dwarfs, and their relevance to cataclysmic variables. Particular attention is given to helium star cataclysmics which might be the precursors of some Type I supernovae or ultrashort period x-ray binaries. Finally we present new evolutionary calculations using the updated nuclear reaction rates for the formation of O+Ne+Mg white dwarfs, and discuss the composition structure and their relevance to the model for neon novae. 61 refs., 14 figs.
- Research Organization:
- Brookhaven National Lab., Upton, NY (USA)
- DOE Contract Number:
- AC02-76CH00016
- OSTI ID:
- 7131686
- Report Number(s):
- BNL-38863; CONF-8606204-2; ON: DE87004172
- Resource Relation:
- Conference: International Astronomical Union colloquium, Bamberg, F.R. Germany, 16 Jun 1986; Other Information: Paper copy only, copy does not permit microfiche production
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
GENERAL PHYSICS
WHITE DWARF STARS
STAR EVOLUTION
BINARY STARS
CHANDRASEKHAR THEORY
HELIUM BURNING
MAGNESIUM
NEON
NEUTRON STARS
OXYGEN
STAR ACCRETION
SUPERNOVAE
X RADIATION
ALKALINE EARTH METALS
DWARF STARS
ELECTROMAGNETIC RADIATION
ELEMENTS
ERUPTIVE VARIABLE STARS
FLUIDS
GASES
IONIZING RADIATIONS
METALS
NONMETALS
RADIATIONS
RARE GASES
STAR BURNING
STARS
VARIABLE STARS
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources