2000/06/23 by Kohji Tomisaka, Tomisaka, Kohji
Physics and Astronomy · #Astro and Planetary Science #Astrophysics (astro-ph) #Astrophysics and Star Formation Studies #FOS: Physical sciences #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0006329
4 pages, presented in IAU symposium #200 "The Formation of Binary Stars" at Potsdam, Germany; April 10-15 2000
arxiv created 2000/06/23 · openalex publication_date 2000/06/23 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Dynamical contraction of a slowly-rotating magnetized cloud is studied using the magnetohydrodynamical (MHD) simulations. In the isothermal stage (n \la n\rm A ∼ 1010\rm cm-3), the cloud evolves similarly to that expected from Larson-Penston self-similar solution and experiences the run-away collapse. However, after the central density exceeds ∼ n\rm A, an accretion disk is formed around the adiabatic core. Just outside the core, outflow is ejected by the effect of magnetic torque (magnetocentrifugal wind). Since ∼ 10% of the mass is ejected with almost all the angular momentum, the specific angular momentum of the protostellar core reduces to that observed in main-sequence stars.