The Ṁ–M relationship in pre-main sequence stars
The Ṁ–M relationship in pre-main sequence stars
复制标题
前主序星中的Ṁ-M关系
DOI：
10.1111/j.1745-3933.2006.00177.x
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发表时间：
2006
影响因子：
--
通讯作者：
J. Pringle
中科院分区：
文献类型：
--
作者：
C. Clarke;J. Pringle
我们检查了最近的数据和分析的Natta等人。关于吸积率的年轻恒星作为恒星质量的函数，并得出结论，明显陡峭的吸积率对质量的依赖性是强烈驱动的选择/检测阈值。我们认为，吸积和恒星质量之间的物理关系的令人信服的证明需要进一步的研究，这是纳塔等人的情况下，包括关于上限的信息，并量化样品在低和高吸积率下可能的不完整性。我们指出，在平面中的检测分布原则上可以用来测试传统的吸积盘演化模型，更高的灵敏度的意见可能能够测试的假设，加速光盘清除在晚些时候。
We examine the recent data and analysis of Natta et al. concerning the accretion rate on to young stars as a function of stellar mass, and conclude that the apparently steep dependence of accretion rate on mass is strongly driven by selection/detection thresholds. We argue that a convincing demonstration of a physical relationship between accretion and stellar mass requires further studies which, as is the case for Natta et al., include information on upper limits, and which quantify the possible incompleteness of the sample, at both low and high accretion rates. We point out that the distribution of detections in the -plane can in principle be used to test conventional accretion disc evolutionary models, and that higher sensitivity observations might be able to test the hypothesis of accelerated disc clearing at late times.