SpringerLink
ForumSpringerAstron. Astrophys.
ForumWhats NewSearchOrders


Astron. Astrophys. 325, 569-584


Table of Contents
Available formats: HTML | PDF | (gzipped) PostScript

Dust evolution in protoplanetary accretion disks

Wolfgang Schmitt, Thomas Henning, and Rastislav Mucha

Max Planck Society, Research Unit ``Dust in Star-forming Regions'', Schillergäßchen 2-3, D-07745 Jena, Germany

Received 3 December 1996 / Accepted 28 March 1997

Abstract

The time evolution of dust particles in circumstellar disk-like structures around protostars and young stellar objects was investigated. For the first time, we coupled the dust evolution directly to the evolution of the disk and followed the influence of opacity changes due to collisional aggregation on the dynamics of the disk. For that purpose, we numerically simulated the dynamical evolution of a turbulent protoplanetary accretion disk described by a time-dependent one-dimensional (radial) ``alpha'' model. Within this model, the growth of dust grains due to coagulation was calculated by solving numerically the non-linear Smoluchowski equation. As physical processes leading to relative velocities between the grains, Brownian motion, turbulence, and drift motion were taken into account. In contrast to other studies, we especially considered particle-cluster agglomeration (PCA) as growth mode but also included cluster-cluster agglomeration (CCA) into our considerations. For time periods of 100 years and disk radii up to 100 AU, the mass distributions of coagulated dust grains were calculated. From these mass spectra, we determined the corresponding Rosseland mean dust opacities. The variations of the dust grain opacity drive changes in the energetic structure of the protoplanetary disk which again influences the accretion process itself. Our results show three evolutionary stages of the PCA process. For CCA particles, there is no dust growth after the disappearance of the smallest grains. The different characteristic timescales for the coagulation at different radii result in the restructuring of the dust region of the protoplanetary disks. Significant changes in the thermal and optical structure of the disk occur.

Key words: accretion disks - hydrodynamics - turbulence - methods: numerical - solar system: formation - planetary system


© European Southern Observatory (ESO) 1997

Online publication: September 9, 1997
Last change: April 28, 1998
helpdesk.link@springer.de