SCYON Abstract

Received on February 14 2007

Rotational Velocities For B0-B3 Stars in 7 Young Clusters:
Further Study of the Relationship between Rotation Speed and
Density in Star-Forming Regions

AuthorsS. C. Wolff, S. E. Strom, and D. Dror
Affiliation
National Optical Astronomy Observatory
Accepted byAstronomical Journal
Contactsstrom@noao.edu

swolff@noao.edu
URLhttp://www.arxiv.org/abs/astro-ph/0702133
Links NGC 6823 / NGC 7380 / IC 1805 / NGC 2244 / NGC 6611 / Orion

Abstract

We present the results of a study aimed at assessing the differences in the distribution of rotation speeds, N (v sin i) among young (1-15 Myr) B stars spanning a range of masses 6 < M/M(sun) < 12 and located in different environments: 7 low density (ρ < 1 M (sun) /pc3) ensembles that are destined to become unbound stellar associations, and 8 high density ( ρ >> 1 M (sun) /pc3) ensembles that will survive as rich, bound stellar clusters for ages well in excess of 108 years. Our results demonstrate (1) that independent of environment, the rotation rates for stars in this mass range do not change by more than 0.1 dex over ages t ~ 1 to t ~ 15 Myr; and (2) that stars formed in high density regions lack the cohort of slow rotators that dominate the low density regions and young field stars. We suggest that the differences in N(v sin i) between low and high density regions may reflect a combination of initial conditions and environmental effects: (1) the higher turbulent speeds that characterize molecular gas in high density, cluster- forming regions; and (2) the stronger UV radiation fields and high stellar densities that characterize such regions. Higher turbulent speeds may lead to higher time-averaged accretion rates during the stellar assembly phase. In the context of stellar angular momentum regulation via “disk-locking,” higher accretion rates lead to both higher initial angular momenta and evolution-driven increases in surface rotation rates as stars contract from the birthline to the Zero Age Main Sequence. Stronger UV radiation fields and higher densities may lead to shorter disk lifetimes in cluster-forming regions. If so, B stars formed in dense clusters are more likely to be “released” from their disks early during their PMS lifetimes and evolve into rapid rotators as they conserve angular momentum and spin up in response to contraction. By contrast, the majority of their brethren in low density, association forming regions can retain their disks for much or all of their PMS lifetimes, are “locked” by their disks to rotate at constant angular speed, and lose angular momentum as they contract toward the ZAMS, and thus arrive on the ZAMS as relatively slowly rotating stars