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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.
| Serija: | ESO Astrophysics Symposia |
| Leidėjas: | Springer Berlin Heidelberg |
| Išleidimo metai: | 2014 |
| Knygos puslapių skaičius: | 332 |
| ISBN-10: | 3662224828 |
| ISBN-13: | 9783662224823 |
| Formatas: | 235 x 155 x 19 mm. Knyga minkštu viršeliu |
| Kalba: | Anglų |
Parašykite atsiliepimą apie „The Bottom of the Main Sequence ¿ And Beyond: Proceedings of the ESO Workshop Held in Garching, Germany, 10¿12 August 1994“
