Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...312..624d&link_type=abstract
Astronomy and Astrophysics, v.312, p.624-642
Astronomy and Astrophysics
Astrophysics
39
Accretion Disks, Molecular Processes, Solar System: Formation, Dust
Scientific paper
Slow radial particle transport moves dust grains from the cold outer regions of a protoplanetary accretion disk into its warm central part where grains are destroyed. This paper considers in detail the destruction processes for the silicate and carbon dust component. Silicate dust is shown to vaporize under near equilibrium conditions and carbon dust is shown to undergo a slow combustion by oxidation reactions with OH radicals. A simple and efficient method is outlined for calculating the dust destruction. This method is applied together with a semianalytical approximation for a thin accretion disk to calculate selfconsistent models for a protoplanetary accretion disk taking full account of the strong non-linear coupling between temperature structure, dust destruction processes, and opacity. It is found that carbon dust is the first dust component which disappears at ~2AU where T~950K. The silicate dust component starts vaporization at ~0.6AU at a temperature of T~1650K while the last grains silicate survive down to ~0.07AU where the temperature is T~2100K.
Duschl Wolfgang J.
Gail Hans-Peter
Tscharnuter Werner M.
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