The chemistry of transient dense cores |
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| Authors: | R T Garrod D A Williams T W Hartquist J M C Rawlings S Viti |
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| Institution: | Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT;Department of Physics and Astronomy, University of Leeds, Leeds LS2 9JT |
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| Abstract: | We investigate the chemistry of a transient density fluctuation, with properties similar to those of a dense core within a molecular cloud. We run a multipoint chemical code through a core's condensation from a diffuse medium to its eventual dispersion, over a period of ～1 Myr. We find a significant enhancement of the chemical composition of the core material on its return to diffuse conditions, whilst the expansion of the core as it disperses moves this material out to large distances from the core centre. This process transports molecular species formed in the high-density regions out into the diffuse medium. Chemical enrichment of the cloud as a whole also occurs, as other cores of various sizes, life-spans and separations evolve throughout. Enrichment is strongly affected by freeze-out on to dust grains, which takes place in high-density, high visual extinction regions. As the core disperses after reaching its peak density and the visual extinction drops below a critical value, grain mantles are evaporated back into the gas phase, initiating more chemistry. The influence of the sizes, masses and cycle periods of cores will be large both for the level of chemical enrichment of a dark cloud and ultimately for the low-mass star formation rate. We also consider the case of a self-gravitating core, by holding its peak density conditions for a further 0.4 Myr. We find that the differences are generally small, and the resultant column densities do not provide definitive criteria for detection of this condition. However, increases in fractional abundances due to reinjection of mantle-borne species may provide a criterion for a negative detection. |
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| Keywords: | MHD stars: formation ISM: clouds ISM: molecules |
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