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Chemical Reactions and Dust Destruction in Protoplanetary Accretion Disks

Published online by Cambridge University Press:  27 February 2018

Frédéric Finocchi ,
Hans-Peter Gail ,
Wolfgang J. Duschl  and
Werner M. Tscharnuter
Frédéric Finocchi
Affiliation:
Institut für Theoretische Astrophysik, Universität Heidelberg, Tiergartenstr. 15, D-69121 Heidelberg, Germany
Hans-Peter Gail
Affiliation:
Institut für Theoretische Astrophysik, Universität Heidelberg, Tiergartenstr. 15, D-69121 Heidelberg, Germany
Wolfgang J. Duschl
Affiliation:
Institut für Theoretische Astrophysik, Universität Heidelberg, Tiergartenstr. 15, D-69121 Heidelberg, Germany Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany
Werner M. Tscharnuter
Affiliation:
Institut für Theoretische Astrophysik, Universität Heidelberg, Tiergartenstr. 15, D-69121 Heidelberg, Germany

Abstract

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A nonequilibrium calculation for the chemistry in a classical protoplanetary accretion disk is presented. Slow radial particle transport moves grains from the cold outer regions of a protoplanetary accretion disk into its warm central part where grains are destroyed. We consider the destruction processes for the silicate and carbon dust component and follow the chemical composition of the gas as a function of the radial distance from the protostar. The main result of this calculation is the presence of huge amounts of methane at a distance of ~ 1 AU from the protostar as product of the carbon dust destruction. It is very likely that more complex organics also are present' in this region.

Type
XIII. Relationships to Interstellar Dust
Information
International Astronomical Union Colloquium , Volume 150: Physics, Chemistry and Dynamics of Interplanetary Dust , 1996 , pp. 517 - 524
Copyright
Copyright © Astronomical Society of the Pacific 1996

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