恒星和星团的质量损失和演化：个人的历史观点
Mass Loss and Evolution of Stars and Star Clusters: a Personal Historical Perspective
摘要：
从个人的历史观点出发，讨论了从1965年到现在，热星风和热星质量损失研究的发展和进展。目前状态的知识恒星风，在本次研讨会上提出的论文的基础上，进行了说明。大约10年前，恒星风的机制已相当清楚，质量损失率也已为人所知，而考虑质量损失的恒星演化理论的预测也与观测相符。然而，最近的研究，特别是那些基于FUSE观测，导致了显着减少的质量损失率，不同意从辐射驱动的风模型的预测。这种情况进行了讨论，并提出了未来的研究，可以澄清这种情况。我还讨论了已知的星团在不同环境中的溶解。溶解时间可以从簇样品的质量和年龄分布中得到。由此产生的溶解时间的集群在太阳附近（SN）和相互作用的星系短于预测的两体松弛的集群在潮汐场。与巨大分子云的相遇可以解释SN中星系团的命运，并且是相互作用星系中星系团寿命短的最可能原因。
英文摘要：
The development and progress of the studies of winds and mass loss from hot stars, from about 1965 up to now, is discussed in a personal historical perspective. The present state of knowledge about stellar winds, based on papers presented at this workshop, is described. About ten years ago the mechanisms of the winds were reasonably well understood, the mass loss rates were known, and the predictions of stellar evolution theory with mass loss agreed with observations. However, recent studies especially those based on FUSE observations, have resulted in a significant reduction of the mass loss rates, that disagrees with predictions from radiation driven wind models. The situation is discussed and future studies that can clarify the situation are suggested. I also discuss what is known about the dissolution of star clusters in different environments. The dissolution time can be derived from the mass and age distributions of cluster samples. The resulting dissolution times of clusters in the solar neighborhood (SN) and in interacting galaxies are shorter than predicted by two-body relaxation of clusters in a tidal field. Encounters with giant molecular clouds can explain the fate of clusters in the SN and are the most likely cause of the short lifetime of clusters in interacting galaxies.
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