Importance of the initial conditions for star formation – II. Fragmentation-induced starvation and accretion shielding

Authors

  • Philipp Girichidis,

    Corresponding author
    1. Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
    2. Cardiff School of Physics and Astronomy, The Parade, Cardiff CF24 3AA
    3. Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany
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  • Christoph Federrath,

    1. Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
    2. Ecole Normale Supérieure de Lyon, CRAL, 69364 Lyon Cedex 07, France
    3. Monash Centre for Astrophysics (MoCA), School of Mathematical Sciences, Monash University, Vic 3800, Australia
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  • Robi Banerjee,

    1. Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany
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  • Ralf S. Klessen

    1. Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
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E-mail: philipp@girichidis.com

ABSTRACT

We investigate the impact of different initial conditions for the initial density profile and the initial turbulence on the formation process of protostellar clusters. We study the collapse of dense molecular cloud cores with three-dimensional adaptive mesh refinement simulations. We focus our discussion on the distribution of the gas among the protostellar objects in the turbulent dynamical cores. Despite the large variations in the initial configurations and the resulting gas and cluster morphology we find that all stellar clusters follow a very similar gas accretion behaviour. Once secondary protostars begin to form, the central region of a cluster is efficiently shielded from further accretion. Hence, objects located close to the centre are starved of material, as indicated by a strong decrease of the central accretion rate. This fragmentation-induced starvation occurs not only in rotationally supported discs and filaments, but also in more spherically symmetric clusters with complex chaotic motions.

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