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Radiation Driven Implosion and Triggered Star Formation

Published online by Cambridge University Press:  27 April 2011

T. G. Bisbas ,
A. P. Whitworth ,
R. Wünsch ,
D. A. Hubber  and
S. Walch
T. G. Bisbas
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic, Boční II 1401, 141 31 Prague, Czech Republic. email: t.bisbas@astro.cf.ac.uk
A. P. Whitworth
Affiliation:
School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, United Kingdom
R. Wünsch
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic, Boční II 1401, 141 31 Prague, Czech Republic. email: t.bisbas@astro.cf.ac.uk
D. A. Hubber
Affiliation:
Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, United Kingdom
S. Walch
Affiliation:
School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, United Kingdom
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Abstract

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We present simulations of stable isothermal clouds exposed to ionizing radiation from a discrete external source, and identify the conditions that lead to Radiatively Driven Implosion and Star Formation. We use the Smoothed Particle Hydrodynamics code SEREN (Hubber et al. 2010) and the HEALPix-based photoionization algorithm described in Bisbas et al. (2009). We find that the incident ionizing flux is the critical parameter determining the evolution; high fluxes disperse the cloud, whereas low fluxes trigger star formation. We find a clear connection between the intensity of the incident flux and the parameters of star formation.

Keywords

hydrodynamicsmethods: numericalstars: formation(ISM:) HII regions
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 263 - 266
Copyright
Copyright © International Astronomical Union 2011

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