一种新的X射线反射模型在V1223人马座上的应用
Application of a new X-ray reflection model to V1223 Sagittarii
摘要：
在中间极星中，白矮星的内禀热辐射是典型的研究对象。很少有报道分析了从WD的X射线反射。我们最近开发了一个精心制作的IP反射光谱模型。在这里，我们报告的第一个应用程序的反射模型与IP热模型的光谱最亮的典型IP V1223人马座观测的朱雀和NuSTAR卫星。该模型合理地再现了5-78 keV范围内的光谱，并估计WD质量为0.92 $\pm$ 0.02 $M_\odot$。该模型估计的WD质量与使用活动星系核反射模型和部分覆盖吸收模型测量的WD质量一致。然而，发现选择不正确的参数值，例如不合适的拟合能带和不正确的金属丰度，会引入系统误差（例如，$<\sim$ 0.2 $M_\odot$（WD质量））。我们的自旋相位分辨分析导致了关于荧光铁K $_α$线的等效宽度和激波后吸积柱与视线（视角）之间的角度的调制的发现。视角与X射线通量近似反相关，并且具有分别为55 $^\circ$和7 $^\circ$的平均和半幅值，其分别从55 $^\circ$和7 $^\circ$的视线指向两个WD自旋轴角。两个估计的自旋轴角都不同于所报告的24 $^\circ$的系统倾角。
英文摘要：
In intermediate polars (IPs), the intrinsic thermal emissions from white dwarfs (WDs) have typically been studied. Few reports have analyzed X-ray reflections from WDs. We recently developed an elaborate IP-reflection spectral model. Herein, we report the first application of a reflection model with an IP thermal model to the spectra of the brightest typical IP V1223 Sagittarii observed by the Suzaku and NuSTAR satellites. The model reasonably reproduces the spectra within the range of 5-78 keV and estimates the WD mass as 0.92$\pm$0.02 $M_\odot$. The WD mass estimated by the proposed model is consistent with that measured using an active galactic nuclei reflection model and a partial covering absorption model. However, the choice of incorrect parameter values, such as an unsuitable fitting energy band and an incorrect metal abundance, was found to introduce systematic errors (e.g., $<\sim$ 0.2 $M_\odot$ in the WD mass) in the WD mass measurement. Our spin phase-resolved analysis resulted in discoveries regarding the modulations of the equivalent width of the fluorescent iron K$_α$ line and the angle between the post-shock accretion column and the line-of-sight (viewing angle). The viewing angle anti-correlates approximately with the X-ray flux and has average and semi-amplitude values of 55$^\circ$ and 7$^\circ$, respectively, which points toward two WD spin axis angles from the line-of-sight of 55$^\circ$ and 7$^\circ$, respectively. Both estimated spin axis angles are different from the reported system inclination of 24$^\circ$.
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