Meridional circulation and turbulence in surface layers of the stars |
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| Authors: | A Z Dolginov V A Urpin |
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| Institution: | 1. A. F. Ioffe Physical and Technical Institute, USSR Academy of Sciences, Leningrad, U.S.S.R.
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| Abstract: | The meridional circulation is considered in the surface layers of the stars where the optical depth τ?1. It is shown that the radial component of circulation velocity reaches its maximum value at τ≈1 and decreases at τ→0. The tangential velocity reverses its sign at τ≈1 — i.e., the meridional flows are closed in stellar atmospheres. The tangential velocities can be of the order of 106–107 cm s?1 in atmospheres of O-B-A stars. Such hydrodynamical motions can result in the generation of turbulence in the surface layers. Characteristic turbulent velocities are of the order of 105–106 cm s?1 in early-type stars. The small-scale turbulent motions generate the acoustic waves and the flux of such waves may be the source of energy to heat coronae in O and B stars. |
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