GX 349+2吸积盘上的电离反射皮
A ionized reflecting skin above the accretion disk of GX 349+2
摘要：
X射线二元光谱的Fe-K α区域中的宽发射特征代表了约束这些系统的几何和物理的宝贵探针。几个含有中子星的低质量X射线双星系统（LMXB）在6 ~ 7 keV之间显示出宽的辐射特征，其中大部分被解释为来自吸积盘内部的反射特征，类似于在含有黑洞候选者的X射线双星系统的光谱中所观察到的特征。NS LMXB GX 349+2由XMM-牛顿卫星观测，由于其高有效面积和6至7 keV之间的良好光谱分辨率，可以对Fe-Ka区域进行详细的光谱研究。我们研究的XMM数据在0.7-10 keV的能量带。连续辐射是由一个黑体组件加上一个多色盘黑体建模。残差中存在1 keV处的非常强的发射线，2.63、3.32、3.9 keV处的三个宽发射特征以及Fe-Ka区域中的更宽发射特征。高于2 keV的宽发射特征可以等效地与高斯分布或相对论性模糊线（XSPEC中的圆盘线）很好地拟合。Fe-Ka特征分别使用6.76 keV处的盘线分量或6.7和6.97 keV处的两个盘线分量更好地拟合。的发射功能被解释为共振跃迁的S XVI，Ar XVIII，Ca XIX，和高度电离的铁。用相对论模糊线模拟线轮廓，我们发现反射等离子体位于距离NS小于40公里处，该值与从多色盘黑体分量（$24 \pm 7$公里）推断的吸积盘的内半径兼容。GX 349+2的倾角在40度和47度之间。
英文摘要：
The broad emission features in the Fe-Kalpha region of X-ray binary spectra represent an invaluable probe to constrain the geometry and the physics of these systems. Several Low Mass X-ray binary systems (LMXBs) containing a neutron star (NS) show broad emission features between 6 and 7 keV and most of them are nowi nterpreted as reflection features from the inner part of an accretion disk in analogy to those observed in the spectra of X-ray binary systems containing a Black Hole candidate. The NS LMXB GX 349+2 was observed by the XMM-Newton satellite which allows, thanks to its high effective area and good spectral resolution between 6 and 7 keV, a detailed spectroscopic study of the Fe-Kalpha region. We study the XMM data in the 0.7-10 keV energy band. The continuum emission is modelled by a blackbody component plus a multicolored disk blackbody. A very intense emission line at 1 keV, three broad emission features at 2.63, 3.32, 3.9 keV and a broader emission feature in the Fe-Kalpha region are present in the residuals. The broad emission features above 2 keV can be equivalently well fitted with Gaussian profiles or relativistic smeared lines (diskline in XSPEC). The Fe-Kalpha feature is better fitted using a diskline component at 6.76 keV or two diskline components at 6.7 and 6.97 keV, respectively. The emission features are interpreted as resonant transitions of S xvi, Ar xviii, Ca xix, and highly ionized iron. Modelling the line profiles with relativistic smeared lines, we find that the reflecting plasma is located at less than 40 km from the NS, a value compatible with the inner radius of the accretion disk inferred from the multicolored disk blackbody component ($24 \pm 7$ km). The inclination angle of GX 349+2 is between 40 and 47 deg.
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