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.

引用

页数：8

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