The core-degenerate scenario for type Ia supernovae

Noam Soker*

*Corresponding author for this work

Research output: Chapter in Book/Report/Conference proceedingConference contributionpeer-review

2 Scopus citations

Abstract

In the core-degenerate (CD) scenario for the formation of Type Ia supernovae (SNe Ia) the Chandrasekhar or super-Chandrasekhar mass white dwarf (WD) is formed at the termination of the common envelope phase or during the planetary nebula phase, from a merger of a WD companion with the hot core of a massive asymptotic giant branch (AGB) star. The WD is destroyed and accreted onto the more massive core. In the CD scenario the rapidly rotating WD is formed shortly after the stellar formation episode, and the delay from stellar formation to explosion is basically determined by the spin-down time of the rapidly rotating merger remnant. The spin-down is due to the magneto-dipole radiation torque. Several properties of the CD scenario make it attractive compared with the double-degenerate (DD) scenario. (1) Off-center ignition of carbon during the merger process is not likely to occur. (2) No large envelope is formed. Hence avoiding too much mass loss that might bring the merger remnant below the critical mass. (3) This model explains the finding that more luminous SNe Ia occur preferentially in star forming galaxies.

Original languageEnglish
Title of host publicationBinary Paths to Type Ia Supernovae Explosions
PublisherCambridge University Press
Pages72-75
Number of pages4
EditionS281
ISBN (Print)9781107019812
DOIs
StatePublished - Jul 2011
Externally publishedYes

Publication series

NameProceedings of the International Astronomical Union
NumberS281
Volume7
ISSN (Print)1743-9213
ISSN (Electronic)1743-9221

Keywords

  • Close binaries
  • Stars: evolution
  • Supernovae

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