通过X射线揭示了DG Tau流出的最快成分
Revealing the fastest component of the DG Tau outflow through X-rays
摘要：
一些金牛座T型星显示出一种特殊的X射线光谱，可以用两种具有不同吸收柱密度的成分来模拟。我们试图解释软X射线成分在DG头，最好的研究这些来源，外流模型，考虑到其他波长的观测。我们通过光谱拟合约束流出属性，并采用简单的半解析公式来描述加热的X射线发射区域的冲击波的属性。X射线的发射与其产生的光学检测流出的最快和最里面的组件是一致的。这种X射线发射部件只需要总质量损失的一小部分。我们喜欢的模型要求冲击波速度在400到500公里/秒之间。当密度大于10^5 /cm ^3时，激波冷却区的所有尺寸都只有几个天文单位，因此即使在光学观测中也无法分辨。这种流出的X射线发射机制也可能在其他吸收较少的金牛T星中起作用，除了日冕和吸积点。
英文摘要：
Some T Tauri stars show a peculiar X-ray spectrum that can be modelled by two components with different absorbing column densities. We seek to explain the soft X-ray component in DG Tau, the best studied of these sources, with an outflow model, taking observations at other wavelengths into consideration. We constrain the outflow properties through spectral fitting and employ simple semi-analytical formulae to describe properties of a shock wave that heats up the X-ray emitting region. The X-ray emission is consistent with its arising from the fastest and innermost component of the optically detected outflow. Only a small fraction of the total mass loss is required for this X-ray emitting component. Our favoured model requires shock velocities between 400 and 500 km/s. For a density >10^5 /cm^3 all dimensions of the shock cooling zone are only a few AU, so even in optical observations this cannot be resolved. This X-ray emission mechanism in outflows may also operate in other, less absorbed T Tauri stars, in addition to corona and accretion spots.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
