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• W2102316596 abstract "We present an analysis of star-forming gas cores in an SPH simulation of a Giant Molecular Cloud. We identify cores using their deep potential wells. This yields a smoother distribution with clearer boundaries than density. Additionally, this gives an indication of future collapse, as bound potential cores (p-cores) represent the earliest stages of fragmentation in molecular clouds. We find that the mass function of the p-cores resembles the stellar IMF and the observed clump mass function, although p-core masses (~0.7 Msol) are smaller than typical density clumps. The bound p-cores are generally subsonic, have internal substructure, and are only quasi-spherical. We see no evidence of massive bound cores supported by turbulence. We trace the evolution of the p-cores forward in time, and investigate the connection between the original p-core mass and the stellar mass that formed from it. We find that there is a poor correlation, with considerable scatter suggesting accretion onto the core is dependent on more factors than just the initial core mass. During the accretion process the p-cores accrete from beyond the region first bound, highlighting the importance of the core environment to its subsequent evolution." @default.
• W2102316596 created "2016-06-24" @default.
• W2102316596 creator A5018186378 @default.
• W2102316596 creator A5018695775 @default.
• W2102316596 creator A5024376393 @default.
• W2102316596 date "2009-06-21" @default.
• W2102316596 modified "2023-10-01" @default.
• W2102316596 title "Fragmentation in molecular clouds and its connection to the IMF" @default.
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• W2102316596 doi "https://doi.org/10.1111/j.1365-2966.2009.14794.x" @default.
• W2102316596 hasPublicationYear "2009" @default.
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