Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.258..107u&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 258, no. 1, Sept. 1, 1992, p. 107-113.
Astronomy and Astrophysics
Astronomy
4
Energy Dissipation, Mixing Length Flow Theory, Stellar Convection, Stellar Cores, Stellar Models, Magnetohydrodynamic Stability, Turbulent Flow, Viscous Flow
Scientific paper
The treatment of turbulent viscous dissipation is improved in the framework of the nonlocal mixing-length theory of Maeder. The larger the turbulent viscous dissipation, the thinner is the convective overshooting region. If the length-scale for the turbulent viscous dissipation is assumed to be equal to the pressure scale-height, a 30-solar-mass model has an overshooting region of moderate extent of about 0.4 Hp1, where Hp1 is the pressure scaleheight at the classical boundary. With this assumption, the extent of overshooting expressed in units of the pressure scaleheight is almost constant but slightly decreases as the evolution proceeds. However, an unstable shell develops in the envelope.
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