Outflow from YSO and Angular Momentum Transfer
| dc.creator | Tomisaka, Kohji | |
| dc.date | 2000-06-23 | |
| dc.date.accessioned | 2026-07-07T01:54:06Z | |
| dc.date.available | 2026-07-07T01:54:06Z | |
| dc.description | Dynamical contraction of a slowly-rotating magnetized cloud is studied using the magnetohydrodynamical (MHD) simulations. In the isothermal stage ($n \la n_{\rm A} \sim 10^{10}{\rm cm}^{-3}$), 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 $\sim n_{\rm A}$, 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 $\sim$ 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. | |
| dc.description | 4 pages, presented in IAU symposium #200 "The Formation of Binary Stars" at Potsdam, Germany; April 10-15 2000 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0006329 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0006329 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/1216 | |
| dc.subject | Astrophysics | |
| dc.title | Outflow from YSO and Angular Momentum Transfer | |
| dc.type | text |