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Collisions of supersonic clouds

Published online by Cambridge University Press:  27 April 2011

Andrew McLeod ,
Jan Palouš  and
Anthony Whitworth
Andrew McLeod
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic Dept. of Physics and Astronomy, Cardiff University, email: [email protected]
Jan Palouš
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic
Anthony Whitworth
Affiliation:
Dept. of Physics and Astronomy, Cardiff University, email: [email protected]
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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.

Keywords

instabilitiesshock wavesISM:cloudsstars: formationstars: mass function
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 355 - 358
Copyright
Copyright © International Astronomical Union 2011

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