Time - dependent CO depletion during the formation of protoplanetary disks


Context. Understanding the gas abundance distribution is essential when tracing star formation using molecular line observations. Changing density and temperature conditions cause gas to freeze-out onto dust grains, and this needs to be taken into account when modeling a collapsing molecular cloud. Aims. This study aims to provide a realistic estimate of the CO abundance distribution throughout the collapse of a molecular cloud. We provide abundance profiles and synthetic spectral lines which can be compared to observations. Methods. We use a 2D hydrodynamical simulation of a collapsing cloud and subsequent formation of a protoplanetary disk as input for the chemical calculations. From the resulting abundances, synthetic spectra are calculated using a molecular excitation and radiation

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@inproceedings{Brinch2008TimeD, title={Time - dependent CO depletion during the formation of protoplanetary disks}, author={C . Brinch and R . J . van Weeren and Michiel R. Hogerheijde}, year={2008} }