The proceedings of this workshop should probably be prefaced with a few words on some of the more confusing jargon. The phrases qVery Low-Mass starq , qVLM starq, or simply qVLMq 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.Neither lab data nor computing power are yet quite equal to the task. Da#39;Antona pointed out that you can tell when your answer is getting close, because slope changes in your HR diagram will line up with those in color-magnitude diagrams ofanbsp;...
|Title||:||The Bottom of the Main Sequence — And Beyond|
|Author||:||Christopher G. Tinney|
|Publisher||:||Springer Science & Business Media - 2013-06-29|