来自RU Lupi的X射线--CTTS中的堆积和风
X-rays from RU Lupi - Accretion and winds in CTTS
摘要：
利用三个XMM-牛顿观测，我们研究了RU Lup的X射线发射，一个吸积和风驱动的CTTS。在与其他明亮的CTTS相比，我们研究可能的签名吸积和风在其X射线发射。结果如下：我们发现三个层次的活动之间的观察RU Lup，明确的磁场起源，由于相应的高等离子体温度。密度分析与OVII三重态表明在冷等离子体的高密度，这表明吸积冲击是一个重要的贡献者的软X射线发射。没有观察到强烈的总体金属消耗。在更活跃的阶段，在6.4千电子伏的过量发射表明铁荧光的存在。在吸积星，我们发现了一个多余的冷等离子体证明较低的OVIII/OVII线比主序星。高密度等离子体似乎只存在于低质量的CTTS中，而中等质量（> 2 M_Sun）的吸积星密度较低。结论：在所有研究的CTTS中，较冷的X射线发射等离子体的特性受到吸积过程的影响。我们怀疑不同的吸积速率和数量的functions，可能与恒星的质量和半径，主要负责不同的性质，他们的冷等离子体成分。RU Lup和其他CTTS异常强的X射线吸收可能与吸积流和从恒星或盘发出的光学透明风有关。
英文摘要：
Using three XMM-Newton observations we study the X-ray emission of RU Lup, a accreting and wind-driving CTTS. In comparison with other bright CTTS we study possible signatures of accretion and winds in their X-ray emission. Results: We find three levels of activity among the observations of RU Lup, clearly of magnetic origin due to the corresponding high plasma temperatures. Density analysis with the OVII triplet indicates high densities in the cool plasma, suggesting accretion shocks to be a significant contributor to the soft X-ray emission. No strong overall metal depletion is observed. Excess emission at 6.4 keV during the more active phase suggest the presence of iron fluorescence. In accreting stars we find an excess of cool plasma as evidenced by lower OVIII/OVII line ratios compared to main-sequence stars. High density plasma appears to be only present in low-mass CTTS, while accreting stars with intermediate masses (> 2 M_Sun) have lower densities. Conclusions: In all investigated CTTS the characteristics of the cooler X-ray emitting plasma are influenced by the accretion process. We suspect different accretion rates and amount of funneling, possibly linked to stellar mass and radius, to be mainly responsible for the different properties of their cool plasma component. The exceptional strong X-ray absorption in RU Lup and other CTTS is probably related to accretion flows and an optically transparent wind emanating from the star or the disk.
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