Chandra observations of the recurrent nova CI Aquilae after its 2000 April outburst

被引:15
|
作者
Greiner, J
Di Stefano, R
机构
[1] Astrophys Inst Potsdam, D-14482 Potsdam, Germany
[2] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany
[3] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[4] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA
来源
ASTROPHYSICAL JOURNAL | 2002年 / 578卷 / 01期
关键词
binaries : close; novae; cataclysmic variables; stars : individual (CI Aquilae); X-rays : stars;
D O I
10.1086/344565
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report the results of two Chandra observations of the recurrent nova CI Aql at 14 and 16 months after its outburst in 2000 April. The X-ray emission is faint in both cases, without any noticeable change in spectrum or intensity. Although the emission is very soft, it is not luminous enough to be due to late-time H burning. This implies that the luminous supersoft phase ended even before the time predicted by the most recent calculations. The details of the X-ray spectrum, together with the fact that the observed X-ray intensity is brighter than preoutburst (1992/1993), suggest that the observed X-ray emission is either due to ionization of the circumstellar material or due to the shocks within the wind and/or with the surrounding medium.
引用
收藏
页码:L59 / L62
页数:4
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