Rotational Velocities for B0-B3 Stars in Seven Young Clusters: Further Study of the Relationship between Rotation Speed and Density in Star-Forming Regions
Citations Over TimeTop 10% of 2007 papers
Abstract
We present the results of a study aimed at assessing the differences in the dis- tribution of rotation speeds, N (v sin i) among young (1-15 Myr) B stars spanning a range of masses 6 > 1 M /pc^3) ensembles that will survive as rich, bound stellar clusters for ages well in excess of 10^8 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.
Related Papers
- → The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets(2023)20 cited
- → Thick disk accretion in Kerr space-time with arbitrary spin parameters(2010)14 cited
- → Accretion from Stellar Winds(1988)1 cited
- → The Effect of Accretion on Young Hierarchical Triple Systems(1997)
- → Angular Momentum Accretion onto Neutron Stars in Wind-fed Binary Systems(2010)