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首页> 外文期刊>The Astrophysical journal >POSSIBILITY OF A WHITE DWARF AS THE ACCRETING COMPACT STAR IN CI CAMELOPARDALIS (=XTE J0421+560)
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POSSIBILITY OF A WHITE DWARF AS THE ACCRETING COMPACT STAR IN CI CAMELOPARDALIS (=XTE J0421+560)

机译：CI CAMELOPARDALIS（= XTE J0421 + 560）中可能有白色矮星作为积聚的紧凑恒星

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We present results from ASCA observations of the binary CI Cam both in quiescence and in outburst in order to identify its central accreting object. The quiescence spectrum of CI Cam consists of soft and hard components, which are separated clearly at around 2-3 keV. A large equivalent width of an iron Kα emission line prefers an optically thin thermal plasma emission model to a nonthermal power-law model for the hard component, which favors a white dwarf as the accreting object, since optically thin thermal hard X-ray emission is a common characteristic among cataclysmic variables (binaries including an accreting white dwarf). However, since the power-law model, which represents the X-ray spectrum of the soft X-ray transients in quiescence, provides an equally good fit to the hard component statistically, we cannot exclude the possibility of a neutron star or a black hole from the quiescence data. The outburst spectrum, on the other hand, is composed of a hard component represented by multitemperature optically thin thermal plasma emission and an independent soft X-ray component that appears below 1 keV intermittently on a decaying light curve of the hard component. The spectrum of the soft component is represented well by a blackbody with the temperature of 0.07-0.12 keV overlaid with several K edges associated with highly ionized oxygen. This, together with the luminosity as high as ～1 x 10~(38) ergs s~(-1), is similar to a supersoft source. The outburst in the hard X-ray band followed by the appearance of the soft blackbody component reminds us of recent observations of novae in outburst. We thus assume that the outburst of CI Cam is that of a nova and obtain the distance to CI Cam of 5-17 kpc by means of the relation between the optical decay time and the absolute magnitude. This agrees well with a recent estimate of the distance of 5-9 kpc in the optical band. All of these results from the outburst data prefer a white dwarf for the central object of CI Cam.
机译：我们提供静态和爆发状态下二元CI Cam的ASCA观测结果，以识别其中央吸积对象。 CI Cam的静态光谱由软组分和硬组分组成，它们在2-3 keV附近清晰地分开。铁Kα发射线的等效宽度大时，对于硬组分，光学上较薄的热等离子体发射模型比非热功率定律模型更优选，这有利于将白矮星作为附着物，因为光学上较薄的热硬X射线发射是灾变变量（二进制文件，包括积聚的白矮星）之间的共同特征。但是，由于幂定律模型可以静态地表示软X射线瞬态的X射线光谱，因此在统计上可以对硬组分提供同样好的拟合，因此我们不能排除中子星或黑洞的可能性从静态数据。另一方面，突出光谱由以多温度光学薄热等离子体发射为代表的硬组分和在硬组分的衰减光曲线上间歇地出现在1keV以下的独立的软X射线组分组成。软组分的光谱很好地由温度为0.07-0.12 keV的黑体表示，黑体上覆盖了多个与高度电离的氧气相关的K边缘。这与高达〜1 x 10〜（38）ers s〜（-1）的发光度相似，类似于超软光源。硬X射线谱带中的爆发，随后出现了柔软的黑体成分，使我们想起了最近对爆发中新星的观测。因此，我们假设CI Cam的爆发是新星爆发，并通过光学衰减时间与绝对大小之间的关系得出距CI Cam的距离为5-17 kpc。这与最近对光波段中5-9 kpc距离的估计非常吻合。来自爆发数据的所有这些结果都更喜欢CI Cam的中心白矮星。

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