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Implementing and comparing sink particles in AMR and SPH

Published online by Cambridge University Press:  27 April 2011

Christoph Federrath ,
Robi Banerjee ,
Daniel Seifried ,
Paul C. Clark  and
Ralf S. Klessen
Christoph Federrath
Affiliation:
Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany email: [email protected]
Robi Banerjee
Affiliation:
Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany email: [email protected]
Daniel Seifried
Affiliation:
Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany email: [email protected]
Paul C. Clark
Affiliation:
Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany email: [email protected]
Ralf S. Klessen
Affiliation:
Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany email: [email protected]
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Abstract

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We implemented sink particles in the Adaptive Mesh Refinement (AMR) code FLASH to model the gravitational collapse and accretion in turbulent molecular clouds and cores. Sink particles are frequently used to measure properties of star formation in numerical simulations, such as the star formation rate and efficiency, and the mass distribution of stars. We show that only using a density threshold for sink particle creation is insufficient in case of supersonic flows, because the density can exceed the threshold in strong shocks that do not necessarily lead to local collapse. Additional physical collapse indicators have to be considered. We apply our AMR sink particle module to the formation of a star cluster, and compare it to a Smoothed Particle Hydrodynamics (SPH) code with sink particles. Our comparison shows encouraging agreement of gas and sink particle properties between the AMR and SPH code.

Keywords

accretionaccretion diskshydrodynamicsISM: kinematics and dynamicsISM: jets and outflowsmethods: numericalshock wavesstars: formationturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 425 - 428
Copyright
Copyright © International Astronomical Union 2011

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