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Collisions of supersonic clouds

Published online by Cambridge University Press:  27 April 2011

Andrew McLeod
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic Dept. of Physics and Astronomy, Cardiff University, email: Andrew.McLeod@astro.cf.ac.uk
Jan Palouš
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic
Anthony Whitworth
Affiliation:
Dept. of Physics and Astronomy, Cardiff University, email: Andrew.McLeod@astro.cf.ac.uk
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Abstract

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We present simulations of supersonic collisions between molecular clouds of mass 500 M and radius 2.24 pc. The simulations are performed with the SEREN SPH code. The code treats the energy equation and the associated transport of heating and cooling radiation. The formation of protostars is captured by introducing sink particles. Low velocity collisions form a shock-compressed layer which fragments to form stars. For high-velocity collisions, υrel ⪆ 5 km s−1, the non-linear thin shell instability strongly disrupts the shock-compressed layer, and may inhibit the formation of stars.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

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