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The birth and death of organic molecules in protoplanetary disks

Published online by Cambridge University Press:  01 February 2008

Thomas Henning  and
Dmitry Semenov
Thomas Henning
Affiliation:
Max Planck Institute for AstronomyKoenigstuhl 17, D-69117 Heidelberg, Germany email: henning@mpia.de, semenov@mpia.de
Dmitry Semenov
Affiliation:
Max Planck Institute for AstronomyKoenigstuhl 17, D-69117 Heidelberg, Germany email: henning@mpia.de, semenov@mpia.de
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Abstract

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The most intriguing question related to the chemical evolution of protoplanetary disks is the genesis of pre-biotic organic molecules in the planet-forming zone. In this contribution we briefly review current observational knowledge of physical structure and chemical composition of disks and discuss whether organic molecules can be present in large amounts at the verge of planet formation. We predict that some molecules, including CO-bearing species such as H2CO, can be underabundant in inner regions of accreting protoplanetary disks around low-mass stars due to the high-energy stellar radiation and chemical processing on dust grain surfaces. These theoretical predictions are further compared with high-resolution observational data and the limitations of current models are discussed.

Keywords

Astrochemistryline: formationmolecular datamolecular processesradiative transfercircumstellar matterplanetary systems: protoplanetary disksstars: pre–main-sequencesubmillimeterX-rays: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S251: Organic Matter in Space , February 2008 , pp. 89 - 98
Copyright
Copyright © International Astronomical Union 2008

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