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Accretion Disks with Convective Viscosity

  • J. Smak (a1)

Abstract

Models of vertical structure are calculated for a range of parameters applicable to dwarf novae with two types of viscosity being included: the standard α-disk viscosity and the additional turbulent viscosity in the convective regions. The resulting surface density (∑) υs. effective temperature (Te ) relations, compared to those without convective viscosity, show larger separation between the two critical points of the ∑ – Te relation, ∑ min and ∑ max . This could suggest that with such a modification the dwarf nova outbursts could be reproduced with a single value of α. (Note that in the standard α approach two different α’s are needed on the hot and cool branch of the ∑ – Te relation, with α cool α hot /4). It turns out, however, that this is not the case. This is due to the fact that additional convective viscosity makes also ∑ max smaller than in the pure α case.

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References

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Accretion Disks with Convective Viscosity

  • J. Smak (a1)

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