The rotation of early B-type stars and the problem of star formation

Details The rotation of early B-type stars and the problem of star formation The rotation of early B-type stars and the problem of star formation

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.210..159g&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 210, Sept. 1, 1984, p. 159-171.

Astronomy and Astrophysics

Astronomy

9

B Stars, Early Stars, Star Formation, Stellar Rotation, Angular Velocity, Maxwell-Boltzmann Density Function, O Stars, Star Clusters, Stellar Luminosity, Velocity Distribution

Scientific paper

Projected rotational velocity distributions (V sin i) are derived for B0-B5 stars in young and in older subgroups of OB associations as well as for field stars. Since known braking mechanisms fail to account for the excess found, which is characterized as a Maxwellian distribution of V and random orientations, the slow rotators may have been formed later, when the subgroups began to disperse. Although stars in tightly bound clusters may have their spin axes nearly perpendicular to the galactic plane, and were probably formed through the collapse and fragmentation of molecular clouds, the formation of stars with random orientations in loose clusters and associations may have been due to the collision of turbulent elements within the clouds.

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