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Observations of the Pipe Nebula have led to the discovery of dense starlesscores. The mass of most cores is too small for their self gravity to hold themtogether. Instead, they are thought to be pressure confined. The observed densecores' mass function (CMF) matches well with the initial mass function (IMF) ofstars in young clusters. Similar CMF's are observed in other star formingregions such as the Aquila Nebula, albeit with some dispersion. The shape ofthese CMF provides important clues to the competing physical processes whichlead to star formation and its feedback on the interstellar media. In thispaper, we investigate the dynamical origin of the the mass function of starlesscores which are confined by a warm, less dense medium. We consider thecoagulation between the cold cores and their ablation due to Kelvin-Helmholtzinstability induced by their relative motion through the warm medium. We areable to reproduce the observed CMF among the starless cores in the Pipe nebula.Our results indicate that in environment similar to the Pipe nebula: 1) beforethe onset of their gravitational collapse, the mass distribution of theprogenitor cores is similar to that of the young stars, 2) the observed CMF isa robust consequence of dynamical equilibrium between the coagulation andablation of cores, and 3) a break in the slope of the CMF is due to theenhancement of collisional cross section and suppression of ablation for coreswith masses larger than the cores' Bonnor-Ebert mass.

On the Coagulation and Size Distribution of Pressure Confined Cores