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Theory of the Star Formation Rate

Published online by Cambridge University Press:  27 April 2011

Paolo Padoan  and
Åke Nordlund
Paolo Padoan
Affiliation:
ICREA & ICC, University of Barcelona, Marti i Franquès 1, E-08028 Barcelona, Spain email: ppadoan@icc.ub.edu
Åke Nordlund
Affiliation:
Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100, Copenhagen, Denmark email: aake@nbi.dk
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Abstract

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This work presents a new physical model of the star formation rate (SFR), tested with a large set of numerical simulations of driven, supersonic, self-gravitating, magneto-hydrodynamic (MHD) turbulence, where collapsing cores are captured with accreting sink particles. The model depends on the relative importance of gravitational, turbulent, magnetic, and thermal energies, expressed through the virial parameter, αvir, the rms sonic Mach number, S,0, and the ratio of mean gas pressure to mean magnetic pressure, β0. The SFR is predicted to decrease with increasing αvir (stronger turbulence relative to gravity), and to depend weakly on S,0 and β0, for values typical of star forming regions (S,0≈4-20 and β0≈1-20). The star-formation simulations used to test the model result in an approximately constant SFR, after an initial transient phase. Both the value of the SFR and its dependence on the virial parameter found in the simulations agree very well with the theoretical predictions.

Keywords

ISM: kinematics and dynamicsMHDstars: formationturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 347 - 354
Copyright
Copyright © International Astronomical Union 2011

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