Other
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21831203o&link_type=abstract
American Astronomical Society, AAS Meeting #218, #312.03; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
The accretion disks around pre-main-sequence stars provide the raw material and initial conditions for the formation of planetary systems. Disk chemistry is thus essential to predict the composition of planetesimals and eventually planets - comet compositions in our own solar system reveal that efficient astrophysical pathways to chemical complexity exists. The chemical evolution is predicted to depend on radiation fields, temperature and density structures. This can be exploited to develop molecular probes of otherwise inaccessible disk processes, and protoplanetary disk chemistry studies typically have the combined objective of constraining how the disk physics drives the disk chemistry, and how the disk chemistry traces the disk physics. Observationally, disk chemistry has been characterized by infrared spectroscopy of the innermost few AUs, far-infrared spectroscopy of the disk atmosphere, and millimeter spectroscopy of the outer disk. This has revealed strong emission from a range of common molecules and ions such as CO, CN, HCN, C2H2, H2O, OH, H2CO, HCO+, N2H+ and DCO+. As expected some lines are found to follow trends with respect to quiescent stellar heating, mass accretion rates, X-ray ionization, and the disk density structure. In response to these observations and in anticipation of more detailed data from especially ALMA, the physical-chemical modeling and theory of disks is the subject of intense efforts. A range of different model approaches have been developed that vary in their treatment of disk structure, radiation fields, and chemical networks. The results stress the importance of UV and X-ray fields as well as the treatment of grain surface chemistry and its relation to gas-phase processes. These recent advances in observations and models of disk chemistry will be reviewed together with current challenges, and the next generation of models, laboratory experiments and observations that will address them.
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