Chemical evolution of turbulent protoplanetary disks

Details Chemical evolution of turbulent protoplanetary disks Chemical evolution of turbulent protoplanetary disks

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007msl..confe.101s&link_type=abstract

"Molecules in Space and Laboratory, meeting held in Paris, France, May 14-18, 2007. Editors: J.L. Lemaire, F. Combes. ISBN: 9782

Astronomy and Astrophysics

Astrophysics

Modelling_Environments

Scientific paper

The importance of turbulent diffusion for disk chemical evolution is discussed. The time-dependent abundances and column densities are modeled with a 1D/2D turbulent mixing chemistry including gas-grain interactions and surface reactions and compared to the results obtained with a static (non-mixing, non-grain growth) model. We find that due to turbulent transport abundances of many observationally important molecules get higher over the disk, in particular in cold midplane, leading to higher column densities than in the static model. A notable exception is the fractional ionization that remains the same in all models. We conclude that the observed column densities in the DM Tau disk fit better with a 2D mixing model.

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