Chemical History of Molecules in Disks

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A protoplanetary disk is a complex chemical mixture of gas and dust. In order to fully understand the disk's chemical composition at the time of planet formation, one has to go back in time and retrace the chemistry to the molecular cloud that collapsed to form the disk and the central protostar. Here we present recent astrochemical observations and models that aim to do just that. The main focus is on water and on simple organic compounds like methanol (CH3OH) and dimethyl ether (CH3OCH3), which are tracers of the organic complexity that likely aided the eventual formation of life. The models predict that water and simple organics were already formed abundantly at an early time. As the parent molecular cloud collapsed and evolved into the protostar + disk system, changes in density, temperature and radiation led to further chemical processing. The abundances of several key species in the models match those observed in comets, but others are off by orders of magnitude. We discuss what both the good and the poor matches mean for the delivery of organic material to the Earth and elsewhere.

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