The Chemical Evolution of Protoplanetary Disks
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1.
University of Michigan–Ann Arbor
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2.
Kobe University
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3.
California Institute of Technology
- 4. Leiden Observatory
Abstract
In this review we reevaluate our observational and theoretical understanding of the chemical evolution of protoplanetary disks. We discuss how improved observational capabilities have enabled the detection of numerous molecules, exposing an active disk chemistry that appears to be in disequilibrium. We outline the primary facets of static and dynamical theoretical chemical models. Such models have demonstrated that the observed disk chemistry arises from warm surface layers that are irradiated by X-ray and FUV emission from the central accreting star. Key emphasis is placed on reviewing areas where disk chemistry and physics are linked, including deuterium chemistry, gas temperature structure, disk viscous evolution (mixing), ionization fraction, and the beginnings of planet formation.
Copyright and License
©2007 University of Arizona Press.
Acknowledgement
E.A.B. thanks L. Hartmann for an initial reading. We also gratefully acknowledge receipt of unpublished
material from 8. Jonkheid, C. Qi, D. Semenov, N. Turner, and K. Willacy. This work was supported by in pa1t by NASA through grants NNG04GH27G and 09374.01-A from STScI, by a Grant-in-Aid for Scientific Research ( 17039008) and "The 21st Century COE Program of the Origin and Evolution of Planetary Systems" from MEXT in Japan, and by a Spinoza award of NWO.
Additional details
- National Aeronautics and Space Administration
- NNG04GH27G
- Space Telescope Science Institute
- 09374.01-A
- Japan Society for the Promotion of Science
- 17039008
- Ministry of Education, Culture, Sports, Science and Technology
- The 21st Century COE Program of the Origin and Evolution of Planetary Systems -
- Dutch Research Council
- Spinoza Award -
- Caltech groups
- Division of Geological and Planetary Sciences
- Publication Status
- Published