Dust in turbulent circumstellar discs

Details Dust in turbulent circumstellar discs Dust in turbulent circumstellar discs

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ap%26ss.200...75v&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 200, no. 1, p. 75-89.

Astronomy and Astrophysics

Astrophysics

1

Accretion Disks, Cosmic Dust, Stellar Envelopes, Turbulence Effects, Astronomical Models, Stellar Winds

Scientific paper

The 'collisional model' for turbulent disks (Hameen-Anttila, 1991) is shown to be equivalent to the alpha model if the same coefficient of viscosity is adopted in both cases and if an unknown numerical coefficient in the former model is chosen appropriately. A combination of both approximations is generalized to include the behavior of dust in the turbulent disk. If the dust grains are not too large, evolution leads to a stable final state having a nonzero temperature. Physical interpretation of the collisional model leads to a new type of turbulence, in which, if a sufficiently large element of gas is randomly displaced even in a stable disk, the resulting oscillations around the equilibrium position are maintained by the orbital energy. This effect produces an irregular wind of 10 to 100 m/s which is sufficient to prevent the sedimentation of dust grains on the equatorial plane.

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