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Radiation-MHD Simulations of HII Region Expansion in Turbulent Molecular Clouds

Published online by Cambridge University Press:  27 April 2011

S. J. Arthur ,
W. J. Henney ,
G. Mellema ,
F. de Colle  and
E. Vázquez-Semadeni
S. J. Arthur
Affiliation:
Centro de Radioastronomía y Astrofísica, UNAM, Campus Morelia, C.P. 58090 Morelia, Michoacán, México
W. J. Henney
Affiliation:
Centro de Radioastronomía y Astrofísica, UNAM, Campus Morelia, C.P. 58090 Morelia, Michoacán, México
G. Mellema
Affiliation:
AlbaNova University Center, Stockholm University, SE-106 91 Stockholm, Sweden
F. de Colle
Affiliation:
Department of Astronomy and Astrophysics, University of California, Santa Cruz
E. Vázquez-Semadeni
Affiliation:
Centro de Radioastronomía y Astrofísica, UNAM, Campus Morelia, C.P. 58090 Morelia, Michoacán, México
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Abstract

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We use numerical simulations to investigate how the expansion of an HII region is affected by an ambient magnetic field. First we consider the test problem of expansion in a uniform medium with a unidirectional magnetic field. We then describe the expansion of an HII region in a turbulent medium, taking as our initial conditions the results of and MHD turbulence simulation. We find that although in the uniform medium case the magnetic field does produce interesting effects over long length and timescales, in the turbulent medium case the main effect of the magnetic field is to reduce the efficiency of fragmentation of the molecular gas.

Keywords

HII regionshydrodynamicsISM: kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 297 - 300
Copyright
Copyright © International Astronomical Union 2011

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