The Bottom of the Main Sequence — And Beyond: Proceedings of the ESO Workshop Held in Garching, Germany, 10–12 August 1994

Christopher G. Tinney (Curatore)

Springer-Verlag Berlin and Heidelberg GmbH & Co. KG, 2014

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.

• Curatore: Christopher G. Tinney
• Editore: Springer-Verlag Berlin and Heidelberg GmbH & Co. KG
• Collana: ESO Astrophysics Symposia
• Anno: 2014
• Rilegatura: Paperback / softback
• Pagine: 309 p.
• Dimensioni: 235 x 155 mm
• EAN: 9783662224823

Testo in English