Supersoft X-ray light curve of RS Ophiuchi (2006)

被引：94
|
作者：
Hachisu, Izumi [1 ]
Kato, Mariko
Manuel Luna, Gerardo Juan
机构：
[1] Univ Tokyo, Coll Arts & Sci, Dept Earth Sci & Astron, Tokyo 1538902, Japan
[2] Keio Univ, Dept Astron, Yokohama, Kanagawa 2238521, Japan
[3] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atomsfer, BR-05508900 Sao Paulo, Brazil
来源：
ASTROPHYSICAL JOURNAL | 2007年 / 659卷 / 02期
关键词：
binaries : close; binaries : symbiotic; novae; cataclysmic variables; stars : individual (RS Ophiuchi); supernovae : general; white dwarfs;
D O I：
10.1086/516838
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
One of the candidates for Type Ia supernova progenitors, the recurrent nova RS Ophiuchi, underwent its sixth recorded outburst in 2006 February, and for the first time a complete light curve of supersoft X-rays has been obtained. It shows the much earlier emergence and longer duration of a supersoft X-ray phase than expected before. These characteristics can be naturally understood when a significant amount of helium layer piles up beneath the hydrogen-burning zone during the outburst, suggesting that the white dwarf (WD) is effectively growing in mass. We have estimated the WD mass in RS Oph to be 1.35 +/- 0.01 M-circle dot, and the growth rate of the WD mass to be at an average rate of similar to 1 x 10(-7) M-circle dot yr (-1). The white dwarf will probably reach the critical mass for Type Ia explosion if the present accretion continues further for a few to several times 10(-5) yr.
引用
收藏
页码：L153 / L156
页数：4
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