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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: [email protected]
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: [email protected]
Michael L. Norman
Affiliation:
Department of Physics, University of California, San Diego, CASS/UCSD 0424, 9500 Gilman Drive, La Jolla, CA 92093-0424, email: [email protected]
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

References

Abel, T., Bryan, G. L. & Norman, M. L. 2000, ApJ 540, 39CrossRefGoogle Scholar
Agertz, O. et al. 2006, astro-ph/0610051Google Scholar
Ballesteros-Paredes, J., Gazol, A., Kim, J., Klessen, R. S., Jappsen, A.-K. & Tejero, E. 2006, ApJ 637, 384CrossRefGoogle Scholar
Beck, R. 2001, Space Science Reviews 99, 243CrossRefGoogle Scholar
Chabrier, G. 2003, PASP 115, 763CrossRefGoogle Scholar
Dobler, W., Haugen, N. E., Yousef, T. A. & Brandenburg, A. 2003, Phys. Rev. Let. 68, 026304Google Scholar
Falkovich, G. 1994, Physics of Fluids 6, 1411CrossRefGoogle Scholar
Han, J. L., Ferriére, K. & Manchester, R. N. 2004, ApJ 610, 820CrossRefGoogle Scholar
Haugen, N. E. & Brandenburg, A. 2004, Phys. Rev. E 70, 026405CrossRefGoogle Scholar
Norman, M. L. & Bryan, G. L. 1999, ASSL Vol. 240: Numerical Astrophysics 19CrossRefGoogle Scholar
Padoan, P. & Nordlund, A. 2002, ApJ 576, 870CrossRefGoogle Scholar
Padoan, P., Juvela, M., Kritsuk, A. & Norman, M. L. 2006, ApJ in pressGoogle Scholar
Palla, F., Salpeter, E. E. & Stahler, S. W. 1983, ApJ 271, 632CrossRefGoogle Scholar
Salpeter, E. E. 1955, ApJ 121, 161CrossRefGoogle Scholar
Stone, J. M. & Norman, M. L. 1992, ApJS 80, 791CrossRefGoogle Scholar
Williams, J. P., de Geus, E. J. & Blitz, L. 1994, ApJ 428, 693CrossRefGoogle Scholar