THE PROGENITORS OF TYPE Ia SUPERNOVAE. I. ARE THEY SUPERSOFT SOURCES?

被引：85
|
作者：
Di Stefano, R. [1 ]
机构：
[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
来源：
ASTROPHYSICAL JOURNAL | 2010年 / 712卷 / 01期
关键词：
binaries: close; planetary nebulae: general; stars: evolution; X-rays: general; X-rays: stars; X-RAY SOURCES; FINAL MASS RELATION; XMM-NEWTON OBSERVATIONS; ACCRETING WHITE-DWARFS; QUASI-SOFT; LUMINOSITY FUNCTION; EXTERNAL GALAXIES; BLACK-HOLE; CHANDRA; NOVAE;
D O I：
10.1088/0004-637X/712/1/728
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
In a canonical model, the progenitors of Type Ia supernovae (SNe Ia) are accreting, nuclear-burning white dwarfs (NBWDs), which explode when the white dwarf reaches the Chandrasekhar mass, M(C). Such massive NBWDs are hot (kT similar to 100 eV), luminous (L similar to 10(38) erg s(-1)), and are potentially observable as luminous supersoft X-ray sources (SSSs). During the past several years, surveys for soft X-ray sources in external galaxies have been conducted. This paper shows that the results falsify the hypothesis that a large fraction of progenitors are NBWDs which are presently observable as SSSs. The data also place limits on sub-M(C) models. While SN Ia progenitors may pass through one or more phases of SSS activity, these phases are far shorter than the time needed to accrete most of the matter that brings them close to M(C).
引用
收藏
页码：728 / 733
页数：6
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