The orbital phase resolved spectroscopy of X-ray binary 4U 1822−371 with Suzaku
The orbital phase resolved spectroscopy of X-ray binary 4U 1822−371 with Suzaku
复制标题
朱雀 X 射线双星 4U 1822−371 的轨道相分辨光谱
DOI：
10.1088/1674-4527/16/4/057
复制
发表时间：
2016
影响因子：
1.8
通讯作者：
L. Ji
中科院分区：
文献类型：
--
作者：
Shu Niu;Shuping Yan;S. Lei;M. Nowak;N. Schulz;L. Ji
4U 1822−371是一颗典型的边缘食型低质量X射线双星，也是吸积盘日冕源的原型。我们报告的结果，在能量范围0.5-45千电子伏观测朱雀在2006年的光谱分析。我们从五个轨道相位提取光谱。光谱可以同样很好地描述了各种先前提出的模型：光学厚模型描述的部分覆盖的截止功率定律和光学薄模型描述的黑体加上截止功率定律。光学厚模型需要约55%的覆盖率，而光学薄模型需要约0.16 keV的中心源的温度。光学厚模型中的光谱也显示了先前用相同的朱雀观测在1030 keV处检测到的回旋加速器线特征。这一特征证实了强磁场的存在。Fe Kα荧光线的强度以及探测到的Fe XXVI强度与我们之前的钱德拉和XMM-牛顿分相光谱分析相似;然而，我们在日食期间也观察到了强Fe XXVI，这表明中央日冕略大。
4U 1822−371 is a typical edge-on eclipsing low mass X-ray binary and the prototype of accretion disk coronal sources. We report on the results of a spectral analysis over the energy range 0.5–45 keV observed by Suzaku in 2006. We extract spectra from five orbital phases. The spectra can be equally well described by various previously proposed models: an optically thick model described by a partially covered cutoff power law and an optically thin model described by a blackbody plus a cutoff power law. The optically thick model requires a covering fraction of about 55%, while the optically thin model requires a temperature of the central source of about 0.16 keV. The spectrum in the optically thick model also shows the previously detected cyclotron line feature at ∼30 keV with the same Suzaku observation. This feature confirms the presence of a strong magnetic field. The Fe Kα fluorescent line strengths as well as the detected Fe XXVI strengths are similar to previous Chandra and XMM-Newton detections in our phased spectral analysis; however, we also observe strong Fe XXVI during the eclipse, which indicates a slightly larger central corona.