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Testing the theory of grain growth and fragmentation by millimeter observations of protoplanetary disks | | T. Birnstiel
; L. Ricci
; F. Trotta
; C.P. Dullemond
; A. Natta
; L. Testi
; C. Dominik
; T. Henning
; C.W. Ormel
; A. Zsom
; | | Date: |
4 Jun 2010 | | Abstract: | Context. Observations at sub-millimeter and mm wavelengths will in the near
future be able to resolve the radial dependence of the mm spectral slope in
circumstellar disks with a resolution of around a few AU at the distance of the
closest star-forming regions.
Aims. We aim to constrain physical models of grain growth and fragmentation
by a large sample of (sub-)mm observations of disks around pre-main sequence
stars in the Taurus-Auriga and Ophiuchus star-forming regions.
Methods. State-of-the-art coagulation/fragmentation and disk-structure codes
are coupled to produce steady-state grain size distributions and to predict the
spectral slopes at (sub-)mm wavelengths.
Results. This work presents the first calculations predicting the mm spectral
slope based on a physical model of grain growth. Our models can quite naturally
reproduce the observed mm-slopes, but a simultaneous match to the observed
range of flux levels can only be reached by a reduction of the dust mass by a
factor of a few up to about 30 while keeping the gas mass of the disk the same.
This dust reduction can either be due to radial drift at a reduced rate or
during an earlier evolutionary time (otherwise the predicted fluxes would
become too low) or due to efficient conversion of dust into larger, unseen
bodies. | | Source: | arXiv, 1006.0940 | | Services: | Forum | Review | PDF | Favorites | |
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