Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981aj.....86..544s&link_type=abstract
ASTRONOMICAL JOURNAL V. 86, P. 544, 1981
Astronomy and Astrophysics
Astronomy
22
Scientific paper
The observational correlation relating peculiar space velocity to stellar mass, wherein the more massive stars have the higher velocities, found in Stone (1979) for the high-velocity (Group H) O-type stars and conservative evolution, is also established for the case where the stellar masses are interpolated from stellar interior models allowing for mass loss from stellar winds. As discussed by Stone (1979, 1981), such a correlation is expected if the Group H stars are produced from supernova explosions in close binary systems. If bolometric magnitudes are used as observables representative of stellar mass, the correlation is also evident and can be given by the approximation V = -34.65 - 10.02Mb for the Group H stars with Mb < -7m.5. Qualitatively, the correlation can also be established independently from radial velocity data alone. Moreover, the Group L (low-velocity O stars) and H stars show striking differences in their frequencies of spectroscopic binaries, inclusion in visual binary or multiple stellar systems, and memberships in associations or young open clusters. Best estimates for these frequencies are 62%:72%:87% for Group Land 21%:0%:33% for Group H. The incidence of Group L stars in single, double, or multiple stellar systems are, respectively, 12%:44%:44%, which suggests that single Group L stars are rare, and that many of these stars were probably born in regions of high gas density leading to multiple star formation. A search for possible H, He, N, and C surface abundance differences between Groups L and H stars was made, but no significant differences were found.
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