Fragmentation and Evolution of Molecular Clouds. I: Algorithm and First Results

Abstract

We present a series of simulations of the fragmentation of a molecular cloud, leading to the formation of a cluster of protostellar cores. The purpose of these simulations is to address a specific numerical problem called artificial fragmentation, that plagues SPH simulations of cloud fragmentation. We argue that this is a serious problem that needs to be addressed, and that the only reasonable and practical way to address it is to use a relatively new technique called particle splitting. Our largest simulation has an effective resolution of 256^3 particles (much higher than most previous SPH simulations of cloud fragmentation) and results in the formation of a dense cluster containing ~3000 protostellar cores. It is the first simulation of this kind to properly resolve the Jeans mass throughout the entire system, at all times, thus preventing artificial fragmentation.

47 pages, 15 figures (2 grayscale, one color), ApJ Suppl, in press

References in corpus (8)

• A Redshift Survey of the Submillimeter Galaxy Population
• Observed Properties of Exoplanets: Masses, Orbits, and Metallicities
• The stellar mass spectrum from non-isothermal gravoturbulent fragmentation
• Resolved Molecular Gas in a Quasar Host Galaxy at Redshift z=6.42
• Photoionising feedback in star cluster formation
• Probing Pre-Protosellar Cores with Formaldehyde
• The Formation of Star Clusters I: 3D Simulations of Hydrodynamic Turbulence
• Centrally condensed turbulent cores: Massive stars or fragmentation?

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