Volume 482, Number 1, April IV 2008
|Page(s)||371 - 385|
|Section||Numerical methods and codes|
|Published online||20 February 2008|
Protostellar collapse: a comparison between smoothed particle hydrodynamics and adaptative mesh refinement calculations
École Normale Supérieure de Lyon, Centre de recherche Astrophysique de Lyon (UMR 5574 CNRS), 46 allée d'Italie, 69364 Lyon Cedex 07, France e-mail: email@example.com
2 Laboratoire AIM, CEA/DSM – CNRS – Université Paris Diderot, IRFU/SAp, 91191 Gif sur Yvette, France
3 Laboratoire de radioastronomie millimétrique (UMR 8112 CNRS), École Normale Supérieure et Observatoire de Paris, 24 rue Lhomond, 75231 Paris Cedex 05, France
Accepted: 16 January 2008
Context. The rapid development of parallel supercomputers is enabling the detailed study of the collapse and the fragmentation of prestellar cores with increasingly accurate numerical simulations. Due to the advances also in sub-millimeter observation technology, we are now able to consider many different modes of low-mass star formation using observations of a range of initials conditions. The challenge for the simulations is to reproduce the observational results.
Aims. Two main numerical methods, namely AMR and SPH, are widely used to simulate the collapse and the fragmentation of prestellar cores. We thoroughly compare these two methods within their standard framework.
Methods. We use the AMR code RAMSES and the SPH code DRAGON. Our simplified physical model consists of an isothermal sphere rotating about the z-axis. First we study the conservation of angular momentum as a function of the resolution. Then, we explore a wide range of simulation parameters to study the fragmentation of prestellar cores.
Results. There appears to be convergence between the two methods, provided numerical resolution in each case is sufficient. We deduced numerical resolution criteria adapted to our physical cases, in terms of resolution per Jeans mass, for an accurate description of the formation of protostellar cores. This convergence is encouraging for future work in simulations of low-mass star formation, providing the aforementioned criteria are fulfilled.
Key words: stars: formation / methods: numerical / hydrodynamics
© ESO, 2008
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