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Theoretical Limits on the Properties of Low-Velocity M-Dwarfs

Published online by Cambridge University Press:  14 August 2015

P. Biermann
P. Biermann*
Affiliation:
Universitäts-Sternwarte Göttingen, F.R.G.

Abstract

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Using a version of the Toomre-criterion (Toomre, 1964) for a mixture of stellar populations, limits are derived for the kinematical properties of the newly discovered population of low-velocity M-dwarfs (Weistrop, 1972; Murray and Sanduleak, 1972); these stars are claimed to be a large mass-fraction (≳ 0.5) of all stars in the solar neighbourhood and to have only 10 km s−1 velocity dispersion. They could make up for the locally missing mass (Oort, 1965; Schmidt, 1974). It is found that a configuration of stellar populations with the M-dwarfs included (having such properties) is not stable in the sense of the Toomre-criterion. The limiting stability properties are given.

Type
Part II/Flattened Systems
Information
Symposium - International Astronomical Union , Volume 69: Dynamics of Stellar Systems , 1975 , pp. 321 - 324
Copyright
Copyright © Reidel 1975 

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