Sign on
ADS Classic is now deprecated. It will be completely retired in October 2019. Please redirect your searches to the new ADS modern form or the classic form. More info can be found on our blog.

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 (591) (Citation History)
· Refereed Citations to the Article
· Associated Articles
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Accreting white dwarf models for type I supernovae. I - Presupernova evolution and triggering mechanisms
Authors:
Nomoto, K.
Publication:
Astrophysical Journal, Part 1, vol. 253, Feb. 15, 1982, p. 798-810. (ApJ Homepage)
Publication Date:
02/1982
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Binary Stars, Stellar Evolution, Stellar Mass Accretion, Stellar Models, Supernovae, White Dwarf Stars, Carbon, Helium, Oxygen
DOI:
10.1086/159682
Bibliographic Code:
1982ApJ...253..798N

Abstract

Results are presented of numerical calculations of the presupernova evolution and triggering mechanisms of accreting white dwarf stars, which have been suggested as the progenitors of type I supernovae. The evolution of carbon-oxygen white dwarf models accreting helium in binary systems was computed using a Henyey-type hybrid method including both thermal and hydrodynamical equations. It is found that type I supernovae can be triggered by the off-center detonation of helium in systems with slow or intermediate accretion rates, or by the central carbon flash for slow or rapid accretion rates. Both helium detonation and carbon deflagration are possible for the case of slow accretion rates due to the importance of initial mass in determining the mode of ignition. Attention is also given to possible mechanisms for the building up of the helium zone surrounding the white dwarf, including direct transfer of helium from the companion star and hydrogen shell burning by processes depending on the accretion rate.

Associated Articles

Part  1     Part  2     Part  3     Part  4    


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