Rotational velocities of low-mass stars in the Pleiades

Details Rotational velocities of low-mass stars in the Pleiades Rotational velocities of low-mass stars in the Pleiades

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...280..202s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-647X), vol. 280, May 1, 1984, p. 202-212.

Astronomy and Astrophysics

Astrophysics

151

Pleiades Cluster, Stellar Evolution, Stellar Mass, Stellar Rotation, Stellar Spectrophotometry, Angular Velocity, Binary Stars, Dwarf Stars, G Stars, Late Stars, Main Sequence Stars, Pre-Main Sequence Stars, Spectrum Analysis, Star Clusters, Variable Stars

Scientific paper

A spectroscopic rotational velocity survey was made of over 60 stars fainter than V = 11 mag in the Pleiades. Most of those stars have rotational velocities below the present detection limit of 10 km/s, but a significant number (18 stars) have v sin i's between 25 and 140 km/s. Based on photometry presented elsewhere, the rapidly rotating stars are identified as heavily spotted main-sequence stars. Thirteen of the 18 rapid rotators are concentrated to a relatively narrow range of color, V-I between 0.95 and 1.35. It is believed those stars stars have only recently arrived on the main sequence and that they owe their high rotational velocities to spin-up while on their radiative pre-main-sequence evolutionary tracks. The G stars in the cluster should also have spun up via that process. Since all of the stars observed with V-I between 0.5 and 0.95 have projected rotational velocities less than 20 km/s, the main sequence spin-down time must be short. The significant number of slow rotators (v sin i less than 10 km/s) in the same color range as the rapid rotators argues for a large range in initial angular momentum and/or an age spread of at least 30 million years among low-mass stars in the Pleiades.

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