S. C. Wolff

TL;DR: In this article, the differences in rotation speeds 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.

TL;DR: In this article, the authors measured rotational velocities of 216 B0--B9 stars in the rich, dense h and chi Persei double cluster, and compared with the distribution of rotational velocity for a sample of field stars having comparable ages and masses, and found that both the higher rotation rates and the pattern of rotation speeds as a function of mass were likely imprinted during the star formation process.

TL;DR: In this article, projected rotational velocities have been measured for a sample of 145 stars with masses between 0.4 and >10 Msun (median mass 2.1 ) located in the Orion star-forming complex.

TL;DR: Chandra observations of solar-like pre-main-sequence (PMS) stars in the Orion flanking fields (FFs) and NGC 2264 (~3 Myr) are compared with the results of the Chandra Orion Ultradeep Project survey of similar objects in the ONC; the correlations between log LX and mass found for PMS stars on convective tracks in these clusters are consistent with the relationships found for the ONc, indicating little change in the median values of either log LX or log LX/Lbol during the first ~3-5 Myr of evolution down conve