Abstract
ABSTRACT It is shown that the velocity dispersion of a large sample of stars can be determined by their distribution on the sky as a function of angular distance from the solar apex. Known or suspected M dwarfs from Gliese's catalog were divided into groups according to distance from the sun, angular distance from the solar apex, whether or not the stars had emission lines, and whether or not they were members of binary or multiple systems. It was found that with this methed only a lower limit of the transverse velocity dispersion could be derived. This value was 13 km sec-1. Based on the present technique and the presently available data, the existence of lowvelocity M dwarfs cannot be ruled out Key words: M dwarfs - stellar motions
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