冷主序星质量损失的经验上限
The empirical upper limit for mass loss of cool main sequence stars
摘要：
冷矮星中由于热成风引起的质量损失率对于模拟主序星和双星的物理参数演化具有重要意义。到目前为止，这种质量损失率的测量很少，有时是相互矛盾的。我们提出了一种新的，独立的方法来测量恒星在过去的生命中失去的质量。它是基于一个疏散星团中太阳型恒星的当前质量分布与计算分布的比较，假设质量低于M（lim）的恒星已经失去了等于DeltaM的质量。DeltaM的实际值或其上限从最佳拟合中找到。分析四个集群：Pleiades，NGC 6996，Hyades和Praesepe在其中三个中给出了DeltaM的上限，而Pleiades的结果是不确定的。对Praesepe星系团得到的最严格的限制表明，该星系团中冷矮星的平均质量损失率低于6 × 10 ^{-11} M（太阳）/年。随着选定的疏散星团的太阳型成员，包括那些光谱类型为K的成员的更精确的质量测定，该方法将为冷矮星的质量损失提供更严格的限制。
英文摘要：
The knowledge of mass loss rates due to thermal winds in cool dwarfs is of crucial importance for modeling evolution of physical parameters of main sequence single and binary stars. Very few, sometimes contradictory, measurements of such mass loss rates exist up to now. We present a new, independent method of measuring an amount of mass lost by a star during its past life. It is based on the comparison of the present mass distribution of solar type stars in an open cluster with the calculated distribution under an assumption that stars with masses lower than M(lim) have lost an amount of mass equal to DeltaM. The actual value of DeltaM or its upper limit is found from the best fit. Analysis of four clusters: Pleiades, NGC 6996, Hyades and Praesepe gave upper limits for DeltaM in three of them and the inconclusive result for Pleiades. The most restrictive limit was obtained for Praesepe indicating that the average mass loss rate of cool dwarfs in this cluster was lower than 6x10^{-11} M(sun)/yr. With more accurate mass determinations of the solar type members of selected open clusters, including those of spectral type K, the method will provide more stringent limits for mass loss of cool dwarfs.
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