由XMM-牛顿卫星观测的矮新星HT CAS的X射线食：光谱和时间分析
The X-ray eclipse of the dwarf nova HT CAS observed by the XMM-Newton satellite: spectral and timing analysis
摘要：
激变变星是由白矮星组成的双星系统，它通过罗氏瓣机制从次级天体吸积物质。在观测时间足够长的情况下，可以进行详细的时间分析，从而确定双星系统的物理性质。我们提出了一个XMM-牛顿观测矮新星HT Cas获得解决的双星系统日食和约束观察到的X射线的起源。我们还将我们的结果与之前的ROSAT和ASCA数据进行比较。在对三台EPIC相机信号进行光谱分析之后，利用已知技术研究了观测到的X射线光变曲线，并获得了日食接触点。X射线谱可以通过温度$kT_1=6.89 \pm 0.23$ keV的热韧致辐射加上温度为$kT_2=30_{-6}^{+8}$ eV的黑体分量（上限）来描述。忽略黑体，辐射热吸收校正通量为$F^{\rm{Bol}}=(6.5\pm 0.1)\times10^{-12}$ erg s $^{-1}$ cm $^{-2}$，对于131 pc的HT Cas距离，对应于辐射热光度$(1.33\pm 0.02)\times10^{31}$ erg s $^{-1}$。对EPIC光变曲线中的食的研究使我们能够限制X射线发射区的大小和位置，结果接近白矮星半径。我们测量的X射线食比相应的光学食稍小（但仅在$\simeq 1.5 σ$的水平上）。如果是这样的话，我们可能已经确定了高纬度发射或一层X射线发射材料的特征，部分被吸积盘所掩盖。
英文摘要：
A cataclysmic variable is a binary system consisting of a white dwarf that accretes material from a secondary object via the Roche-lobe mechanism. In the case of long enough observation, a detailed temporal analysis can be performed, allowing the physical properties of the binary system to be determined. We present an XMM-Newton observation of the dwarf nova HT Cas acquired to resolve the binary system eclipses and constrain the origin of the X-rays observed. We also compare our results with previous ROSAT and ASCA data. After the spectral analysis of the three EPIC camera signals, the observed X-ray light curve was studied with well known techniques and the eclipse contact points obtained. The X-ray spectrum can be described by thermal bremsstrahlung of temperature $kT_1=6.89 \pm 0.23$ keV plus a black-body component (upper limit) with temperature $kT_2=30_{-6}^{+8}$ eV. Neglecting the black-body, the bolometric absorption corrected flux is $F^{\rm{Bol}}=(6.5\pm 0.1)\times10^{-12}$ erg s$^{-1}$ cm$^{-2}$, which, for a distance of HT Cas of 131 pc, corresponds to a bolometric luminosity of $(1.33\pm 0.02)\times10^{31}$ erg s$^{-1}$. The study of the eclipse in the EPIC light curve permits us to constrain the size and location of the X-ray emitting region, which turns out to be close to the white dwarf radius. We measure an X-ray eclipse somewhat smaller (but only at a level of $\simeq 1.5 σ$) than the corresponding optical one. If this is the case, we have possibly identified the signature of either high latitude emission or a layer of X-ray emitting material partially obscured by an accretion disk.
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