软极RS Caeli的相分辨X射线能谱和能谱能量分布
Phase-resolved X-ray spectroscopy and spectral energy distribution of the X-ray soft polar RS Caeli
摘要：
RS Cae是我们对软X射线主导的极星进行的XMM-牛顿观测系列中的第三个目标。我们的观测活动旨在更好地理解和描述多波长数据，系统组件的物理特性，以及RS Cae组件通量的短期和长期行为。我们采用恒星大气，分层吸积柱，和广泛使用的X射线光谱模型。我们拟合了XMM-牛顿光谱，模拟了多波段光变曲线，并选择了光谱能量分布的基本一致的描述。结果软X射线发射明显地主导了RS Cae的XMM-牛顿数据。X射线光变曲线是由主吸积区的辐射形成的，在整个轨道周期内都可以看到，只有流食中断。光学光变曲线由回旋加速器和流发射形成。XMM-牛顿X射线谱在36 eV和7 keV的平均温度下包括类黑体和等离子体成分。光谱拟合给出了部分吸收和反射分量的证据。多温度模型，涵盖了更广泛的温度范围内的X射线发射吸积区域，适当地再现光谱。包括档案数据，我们描述的光谱能量分布与模型的组合的基础上一致的一组参数，并得出一个下限估计的距离d > 750 pc。结论.高辐射热软硬通量比和（X射线）光变曲线的短期变化是非均匀吸积的特征。与硬X射线通量相比，RS Cae显然属于显示出非常强的软X射线通量的极群。在XMM-Newton和ROSAT观测期间，不同的黑体通量和相似的硬X射线和光学通量表明软和硬X射线发射没有直接相关。
英文摘要：
RS Cae is the third target in our series of XMM-Newton observations of soft X-ray-dominated polars. Our observational campaign aims to better understand and describe the multiwavelength data, the physical properties of the system components, and the short- and long-term behavior of the component fluxes in RS Cae. We employ stellar atmosphere, stratified accretion-column, and widely used X-ray spectral models. We fit the XMM-Newton spectra, model the multiband light curves, and opt for a mostly consistent description of the spectral energy distribution. Results. Our XMM-Newton data of RS Cae are clearly dominated by soft X-ray emission. The X-ray light curves are shaped by emission from the main accretion region, which is visible over the whole orbital cycle, interrupted only by a stream eclipse. The optical light curves are formed by cyclotron and stream emission. The XMM-Newton X-ray spectra comprise a black-body-like and a plasma component at mean temperatures of 36eV and 7keV. The spectral fits give evidence of a partially absorbing and a reflection component. Multitemperature models, covering a broader temperature range in the X-ray emitting accretion regions, reproduce the spectra appropriately well. Including archival data, we describe the spectral energy distribution with a combination of models based on a consistent set of parameters and derive a lower limit estimate of the distance d > 750pc. Conclusions. The high bolometric soft-to-hard flux ratios and short-term variability of the (X-ray) light curves are characteristic of inhomogeneous accretion. RS Cae clearly belongs in the group of polars that show a very strong soft X-ray flux compared to their hard X-ray flux. The different black-body fluxes and similar hard X-ray and optical fluxes during the XMM-Newton and ROSAT observations show that soft and hard X-ray emission are not directly correlated.
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