Hostname: page-component-cd9895bd7-8ctnn Total loading time: 0 Render date: 2024-12-25T12:27:08.824Z Has data issue: false hasContentIssue false

Outflow from Protostars and Angular Momentum Transfer

Published online by Cambridge University Press:  13 May 2016

Kohji Tomisaka*
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181–8588, Japan

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Dynamical contraction of a slowly-rotating magnetized cloud is studied using 2D magnetohydrodynamical (MHD) simulations. In the isothermal stage (nnA ∼ 1010cm−3), the cloud evolves similarly to that expected from the Larson-Penston self-similar solution and experiences a run-away collapse. However, after the central density exceeds ∼ nA, an accretion disk is formed around an adiabatic core. Just outside the core, an outflow is ejected by the effect of magnetic torque (magneto-centrifugal 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 pre-main-sequence stars.

Type
IX. Theoretical Context - Detailed Calculations
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Blandford, R. D., & Payne, D. G. 1982, MNRAS, 199, 883.Google Scholar
Ebert, R., von Hoerner, S., & Temesvary, S. 1960, Die Entstehung von Sternen durch Kondensation diffuser Materie (Berlin: Springer), 315.Google Scholar
Larson, R. B. 1969, MNRAS, 145, 271.Google Scholar
Norman, M. L., Wilson, J. R., & Barton, R. T. 1980, ApJ, 239, 968.Google Scholar
Tomisaka, K. 1998, ApJL, 502, L163.Google Scholar