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Dust Evolution in Protoplanetary Accretion Disks

Published online by Cambridge University Press:  12 April 2016

Th. Henning ,
W. Schmitt  and
R. Mucha
Th. Henning
Affiliation:
Max Planck Society, Research Unit “Dust in Star-forming Regions”, Schillergäβchen 3, D-07745 Jena, Germany
W. Schmitt
Affiliation:
Max Planck Society, Research Unit “Dust in Star-forming Regions”, Schillergäβchen 3, D-07745 Jena, Germany
R. Mucha
Affiliation:
Max Planck Society, Research Unit “Dust in Star-forming Regions”, Schillergäβchen 3, D-07745 Jena, Germany

Abstract

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We have numerically investigated the dust evolution in a protoplanetary accretion disk which is described by a time-dependent one-dimensional (radial) α-model. The coagulation of particles due to cohesive collisions is calculated by solving the non-linear Smoluchowski equation. The feedback of the dust evolution and the related opacity changes to the disk evolution is explicitly treated. Three different regimes during the evolution of the grain population can be identified.

Type
Part 15. Poster Papers
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 721 - 722
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

Henning, Th., Stognienko, R. 1996, A&A, 311, 291 Google Scholar
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Schmitt, W., Henning, Th., Mucha, R. 1996, A&A, submittedGoogle Scholar
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