SUZAKU OBSERVATION OF THE CLASSICAL NOVA V2491 Cyg IN QUIESCENCE

被引：16
|
作者：
Zemko, P. [1 ]
Mukai, K. [2 ,3 ,4 ]
Orio, M. [5 ,6 ]
机构：
[1] Univ Padua, Dept Phys & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy
[2] NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
[3] NASA Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA
[4] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA
[5] INAF Osservatorio Padova, I-35122 Padua, Italy
[6] Univ Wisconsin, Dept Astron, Madison, WI 53704 USA
来源：
ASTROPHYSICAL JOURNAL | 2015年 / 807卷 / 01期
关键词：
novae; cataclysmic variables; X-rays: binaries; X-rays: individual (V2491 Cyg); X-RAY OBSERVATIONS; INTERMEDIATE POLARS; RECURRENT NOVAE; WHITE-DWARFS; SPECTRAL-ANALYSIS; LIGHT-CURVE; POST-NOVA; EMISSION; LINE; MATTER;
D O I：
10.1088/0004-637X/807/1/61
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present the Suzaku XIS observation of V2491 Cyg (Nova Cyg 2008 No. 2) obtained in quiescence, more than two years after the outburst. The nova was detected as a very luminous source in a wide spectral range from soft to hard X-rays. A very soft blackbody-like component peaking at 0.5 keV indicates that we observe either remaining, localized hydrogen burning on the surface of the white dwarf, or accretion onto a magnetized polar cap. In the second case, V2491 Cyg is a candidate "soft intermediate polar." We obtained the best fit for the X-ray spectra with several components: two of thermal plasma, a blackbody and a complex absorber. The latter is typical of intermediate polars. The X-ray light curve shows a modulation with a period of similar to 38 minutes. The amplitude of this modulation is strongly energy-dependent and reaches a maximum in the range 0.8-2.0 keV. We discuss the origin of the X-ray emission and pulsations, and the likelihood of the intermediate polar scenario.
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页数：8
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