论文标题
X射线排放从WR 140碰撞的恒星风建模
Colliding stellar wind modelling of the X-ray emission from WR 140
论文作者
论文摘要
我们在标准碰撞恒星风（CSW）图片的框架中对大量二进制WR 140的Chandra和Rxte X射线光谱进行了建模。与具有完整温度均衡的X射线数据相比，在冲击阵线上具有部分电子加热的模型是X射线数据的更好表示。 CSW区域X射线血浆的排放度量在围绕Periastron附近的轨道阶段显示出大量降低。这等同于二元轨道上可变的有效质量损失率。在Periastron附近的轨道阶段，存在于WR 140中的恒星风中过量的相当大的X射线吸收。标准CSW模型提供了线条配置文件，通常与WR 140的X射线频谱中观察到的强线特征的线条配置文件很好地匹配。可变有效的质量损失率可以在CSW的CSW图片中被定性地理解，这些图片的易变恒星风能有效地溶解在Apastron附近的CSW区域，但在Periastron中没有有效地溶解。但是，可能需要使用非球面恒星风的CSW模型的未来开发，以在理论和观察之间获得更好的对应关系。
We modelled the Chandra and RXTE X-ray spectra of the massive binary WR 140 in the framework of the standard colliding stellar wind (CSW) picture. Models with partial electron heating at the shock fronts are a better representation of the X-ray data than those with complete temperature equalization. Emission measure of the X-ray plasma in the CSW region exhibits a considerable decrease at orbital phases near periastron. This is equivalent to variable effective mass-loss rates over the binary orbit. At orbital phases near periastron, a considerable X-ray absorption in excess to that from the stellar winds in WR 140 is present. The standard CSW model provides line profiles that in general do not match well the observed line profiles of the strong line features in the X-ray spectrum of WR 140. The variable effective mass-loss rate could be understood qualitatively in CSW picture of clumpy stellar winds where clumps are efficiently dissolved in the CSW region near apastron but not at periastron. However, future development of CSW models with non-spherically-symmetric stellar winds might be needed to get a better correspondence between theory and observations.
