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Dust in turbulent circumstellar discs

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Abstract

The ‘collisional model’ for turbulent discs (Hämeen-Anttila, 1991) is shown to be equivalent to the α 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 behaviour of dust in the turbulent disc. If the dust grains are not too large, evolution leads to a stable final state having a non-zero 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 disc, 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−1 which is sufficient to prevent the sedimentation of dust grains on the equatorial plane.

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Authors and Affiliations

  1. Department of Astronomy, University of Oulu, Finland

    M. Verronen, H. Vanhala & K. A. Hämeen-Anttila

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  1. M. Verronen
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  2. H. Vanhala
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  3. K. A. Hämeen-Anttila
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Verronen, M., Vanhala, H. & Hämeen-Anttila, K.A. Dust in turbulent circumstellar discs. Astrophys Space Sci 200, 75–89 (1993). https://doi.org/10.1007/BF00658111

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  • DOI: https://doi.org/10.1007/BF00658111

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