Single star progenitors for type Ia supernovae

被引：0

作者：

Tout, Christopher A. ^{[1
]}

Wickramasinghe, Dayal T. ^{[2
]}

Lattanzio, John C. ^{[3
]}

机构：

[1] Observ, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[2] Australian Natl Univ, Dept Math, Canberra, ACT 0200, Australia

[3] Monash Univ, Sch Math, Ctr Stellar & Planetary Astrophys, Clayton, Vic 3800, Australia

来源：

UNSOLVED PROBLEMS IN STELLAR PHYSICS: A CONFERENCE IN HONOUR OF DOUGLAS GOUGH | 2007年 / 948卷

关键词：

stars : AGB and post-AGB; stars : mass-loss; supernovae : general; white dwarfs;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Type Ia supernovae are identified as exploding degenerate stars. Their luminosity is due to the radioactive decay of about a solar mass of Ni-56 through (CO)-C-56 to Fe-56. Although it is generally accepted that a degenerate carbon/oxygen white dwarf explodes as it accretes material from a binary companion, the progenitors of type Ia supernovae have not been categorically identified. The cores of intermediate mass asymptotic giant branch stars are composed of carbon and oxygen in a degenerate state. We discuss conditions under which carbon can ignite at the centre of such a core and when the ensuing explosion would appear as a type Ia supernova.

引用

页码：381 / +

页数：2

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