The Role of Complex Ionized Absorbers in the Soft X-Ray Spectra of Intermediate Polars
The Role of Complex Ionized Absorbers in the Soft X-Ray Spectra of Intermediate Polars
复制标题
复合电离吸收剂在中间极性软 X 射线光谱中的作用
DOI：
10.3847/1538-4357/ac134e
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发表时间：
2021
期刊：
影响因子：
--
通讯作者：
K. Mukai
中科院分区：
文献类型：
--
作者：
N. Islam;K. Mukai
在磁激变变星（mCV）中，X射线辐射源自白色矮星表面附近激波后区域的激波加热的多温度等离子体。这些X射线被激波前区域内吸收体的复杂分布所改变。这些mCV的软X射线光谱中的光电离线和温暖的吸收体功能的存在表明，这些吸收体电离。我们开发了电离复合吸收体模型zxipab，它是由一个幂律分布的电离吸收体在预激波流。使用电离吸收体模型zxipab沿着与冷却流模型的反射组件，我们模拟的宽带钱德拉/高能透射光栅（HETG）和核光谱望远镜阵列（努斯塔）光谱的两个中间极（IP）：NY Lup和V1223 Sgr。我们发现，这个模型很好地描述了许多的H-和He-样的发射线从中等Z元素，这是由碰撞激发等离子体。然而，该模型未能解释一些来自中Z元素的类氦三重态，这指向它们的光电离起源。我们没有找到令人信服的证据，黑体组件来模拟软过剩的钱德拉/HETG光谱的残差中看到的，这可能是由于在估计这些源的星际吸收使用钱德拉/HETG数据和/或多余的通量看到在一些光电离的发射线不占冷却流模型的不确定性。我们描述了这个模型的影响相对于这两个IP的预冲击区域的几何形状。
In magnetic cataclysmic variables (mCVs), X-ray radiation originates from a shock-heated, multi-temperature plasma in the post-shock region near the white dwarf’s surface. These X-rays are modified by a complex distribution of absorbers in the pre-shock region. The presence of photoionized lines and warm absorber features in the soft X-ray spectra of these mCVs suggests that these absorbers are ionized. We developed the ionized complex absorber model zxipab, which is represented by a power-law distribution of ionized absorbers in the pre-shock flow. Using the ionized absorber model zxipab along with a cooling flow model with a reflection component, we model the broadband Chandra/High-Energy Transmission Grating (HETG) and Nuclear Spectroscopic Telescope Array (NuSTAR) spectra of two intermediate polars (IPs): NY Lup and V1223 Sgr. We find that this model describes well many of the H- and He-like emission lines from medium-Z elements, which arise from a collisionally excited plasma. However the model fails to account for some of the He-like triplets from the medium-Z elements, which points toward their photoionized origin. We do not find compelling evidence for a blackbody component to model the soft excess seen in the residuals of the Chandra/HETG spectra, which could be due to uncertainties in the estimation of the interstellar absorption of these sources using the Chandra/HETG data and/or excess fluxes seen in some photoionized emission lines which are not accounted for by the cooling flow model. We describe the implications of this model with respect to the geometry of the pre-shock region for these two IPs.
两个带有软 X 射线组件的新型中间极轴
影响因子：
6.5
作者：
Anzolin G
通讯作者：
Anzolin G