| 书目名称 | The Bottom of the Main Sequence — And Beyond | | 副标题 | Proceedings of the E | | 编辑 | Christopher G. Tinney | | 视频video | | | 丛书名称 | ESO Astrophysics Symposia | | 图书封面 |  | | 描述 | The proceedings of this workshop should probably be prefaced with a few words on some of the more confusing jargon. The phrases "Very Low-Mass star" , "VLM star", or simply "VLM" are now used fairly uniformly by as tronomers studying the stars at the bottom of the hydrogen-burning stellar main sequence - unfortunately, however, there is no clear definition as to what constitutes a VLM star. The reader should be warned that VLM stars are variously considered to be stars with; masses less than 0.3M ; masses 0 less than 0.1M ; spectra later than about M6-7; luminosities fainter than 0 Mv = 15; or luminosities fainter than Mbol = 12. The important features of a VLM star, however, would seem to be (1) that it is about as faint as a star can be, and (2) that it still remains a star (ie. it still burns hydrogen) . All of the above criteria, therefore, would seem to qualify an object as a VLM star, and requiring a more stringent definition is probably quibbling. | | 出版日期 | Conference proceedings 1995 | | 关键词 | Main sequence; cluster; clustering; density; gravitation; gravity; photometry; planet; spectroscopy; star; sta | | 版次 | 1 | | doi | https://doi.org/10.1007/978-3-540-49217-7 | | isbn_softcover | 978-3-662-22482-3 | | isbn_ebook | 978-3-540-49217-7Series ISSN 1431-2433 Series E-ISSN 1611-6143 | | issn_series | 1431-2433 | | copyright | Springer-Verlag Berlin Heidelberg 1995 |
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发表于 2025-3-21 20:01:14
