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The mass distribution of unstable cores in turbulent magnetized clouds

Published online by Cambridge University Press:  01 August 2006

Paolo Padoan ,
Åke Nordlund ,
Alexei G. Kritsuk ,
Michael L. Norman  and
Pak Shing Li
Paolo Padoan
Affiliation:
Department of Physics, University of California, San Diego, CASS/UCSD 0424, 9500 Gilman Drive, La Jolla, CA 92093-0424, email: ppadoan@ucsd.edu
Åke Nordlund
Affiliation:
Astronomical Observatory/NBIfAFG, Juliane Maries Vej 30, DK-2100, Copenhagen, Denmark
Alexei G. Kritsuk
Affiliation:
Department of Physics, University of California, San Diego, CASS/UCSD 0424, 9500 Gilman Drive, La Jolla, CA 92093-0424, email: ppadoan@ucsd.edu
Michael L. Norman
Affiliation:
Department of Physics, University of California, San Diego, CASS/UCSD 0424, 9500 Gilman Drive, La Jolla, CA 92093-0424, email: ppadoan@ucsd.edu
Pak Shing Li
Affiliation:
Astronomy Department, University of California, Berkeley, CA 94720
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Abstract

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The predictions of the Padoan and Nordlund IMF model are tested using the largest simulations of supersonic hydrodynamic (HD) and magneto-hydrodynamic (MHD) turbulence to date (~10003 computational zones). The striking difference between the HD and MHD regimes, predicted by the model, is recovered.

Keywords

star formationIMFturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 283 - 291
Copyright
Copyright © International Astronomical Union 2007

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