Carbon-oxygen white dwarf presupernova models

Details Carbon-oxygen white dwarf presupernova models Carbon-oxygen white dwarf presupernova models

Nov 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982sscr.conf..215c&link_type=abstract

In: Supernovae: A survey of current research; Proceedings of the Advanced Study Institute, Cambridge, England, June 29-July 10,

Computer Science

4

Carbon Stars, Stellar Evolution, Stellar Mass Accretion, Stellar Models, Supernovae, White Dwarf Stars, Binary Stars, Gravitational Collapse, Main Sequence Stars, Neutron Stars, Oxygen

Scientific paper

The long-term evolution of accreting C-O white dwarfs is studied in an attempt to determine the conditions for these objects to be a source of neutron stars and/or Type I supernova events. A binary system consisting of a massive C-O white dwarf and a low-mass main sequence companion is considered. Solidification of the star's core is shown to have two important consequences, the initial exclusion of convection as a mode for burning propagation, and the possible separation of oxygen and carbon with the solid oxygen accumulating in the central regions of the star. Both effects combined with different accretion rates are considered, and it is shown how they can lead to a variety of results ranging from total collapse to partial disruption of the star.

Affiliated with

Also associated with

No associations

Rating

Carbon-oxygen white dwarf presupernova models does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Carbon-oxygen white dwarf presupernova models, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Carbon-oxygen white dwarf presupernova models will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1759133