Mass loaded astronomical flows – II. The chemistry in T-Tauri wind-blown bubbles in dense molecular clouds

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Abstract
In the interior of molecular clouds, the fragmentation of shells bounding T-Tauri wind-driven bubbles forms dense clumps of gas. These clumps are eroded by winds from the next generation of stars, and the erosion loads the wind with H2 and grains on to which heavy elements have been depleted. The chemical evolution of this mass loaded wind is described after its passage through an inward facing shock near the bubble boundary at which sputtering occurs. Molecular accretion on to grain surfaces terminates this chemical evolution; ultimately, material in the subsequently formed clumps is undetectable in the gas phase. Our studies represent an attempt to describe the non-equilibrium chemical evolution in a realistic dynamical scenario which is applicable to regions in which low mass star formation is occurring. If low mass star formation is ubiquitous in observed regions of molecular clouds, the model results have broader implications. The model described here provides a plausible explanation of the high C° abundance and the high C°:CO ratio in molecular clouds, indicates that molecular abundances are in general a function of star forming activity within a cloud, predicts that much material in molecular clouds is observable only in the solid state, and assigns the origin of the large molecular linewidths to motions driven by winds of low mass stars.

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