论文标题
在独特的中间极性paloma中研究复杂的吸收和反射
Study of Complex Absorption and Reflection in a Unique Intermediate Polar Paloma
论文作者
论文摘要
我们使用XMM-Newton和Nustar观测值的同时数据介绍了宽带（0.3-40.0 keV）X射线分析，对独特的中间极性paloma进行了独特的中间极性paloma分析。与自旋期相比，X射线功率光谱在轨道周期内显示出强大的调制。轨道折叠的曲面显示单个宽驼峰结构，具有强度强度的X射线（0.3-10.0 KEV）。能源依赖性下降到$ ϕ \ sim 0.16 $，并且由于复杂的固有吸收剂而出现了0.5 $，强度足以在15 keV左右效果良好。吸收器可能会通过灌木窗帘/积聚流以及由流盘/流磁层相互作用产生的吸收材料造成的。我们注意到吸收剂具有轨道相的显着变化，在轨道相0.1-0.22期间具有最大吸收。吸收器需要多个部分覆盖吸收器成分，并指定使用柱密度分布进行源的光谱建模的必要性。同型冷却流量组件用于建模来自多温度后冲击后区域的发射，使休克温度为$ 31.7 _ { - 3.5}^{+3.3} $ kev，对应于白色dwarf质量为$ 0.74 _ _ _ { - 0.05}^{ - 0.05}^{+0.04}^{+0.04} $ _}我们已经使用了中性吸收剂和温暖的吸收剂模型，这些模型在统计学上具有类似的良好拟合度，但具有不同的物理意义。在Fe K $_α$线复合体中，中性线是最弱的。我们探究了康普顿的反射，并发现光谱拟合中的统计贡献最少，这表明帕洛玛中存在弱反射。
We present the broadband (0.3-40.0 keV) X-ray analysis of a unique intermediate polar Paloma using simultaneous data from XMM-Newton and NuSTAR observatories. The X-ray power spectra show strong modulations over orbital period compared to spin period. The orbit folded lightcurves show single broad hump like structure with strong dips for soft to medium X-rays (0.3-10.0 keV). The energy dependent dips at $ϕ\sim 0.16$ and $0.5$ arise due to complex intrinsic absorber, strong enough to have effect well around 15 keV. The absorber could potentially be contributed from accretion curtain/ accretion stream and absorbing material produced by stream-disc/stream-magnetosphere interactions. We notice significant variation of the absorber with orbital phase, with maximum absorption during orbital phase 0.1-0.22. The absorber requires more than one partial covering absorber component, specifying the necessity to use distribution of column densities for spectral modelling of the source. Isobaric cooling flow component is utilized to model the emission from the multi-temperature post-shock region, giving shock temperature of $31.7_{-3.5}^{+3.3}$keV, which corresponds to white dwarf mass of $0.74_{-0.05}^{+0.04}\;M_{\odot}$. We have used both the neutral absorber and the warm absorber models, which statistically give similarly good fit, but with different physical implications. Among the Fe K$_α$ line complex, the neutral line is the weakest. We probed the Compton reflection, and found minimal statistical contribution in the spectral fitting, suggesting presence of weak reflection in Paloma.
