Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.187..129s&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 187, Apr. 1979, p. 129-144.
Astronomy and Astrophysics
Astronomy
14
Convective Flow, Internal Waves, Stellar Evolution, Stellar Models, Dynamic Stability, Heat Transfer, Prandtl Number
Scientific paper
This paper demonstrates that available oceanographic, laboratory, and theoretical evidence cannot be applied to semiconvection in evolving stars because of a large difference in Prandtl numbers. The onset of convection is investigated by using a linear stability analysis that includes both rotation and magnetic field. It is shown that growing oscillations are possible which have a dispersion relation essentially identical to that of internal waves. Previous laboratory and theoretical finite-amplitude results are examined, a model devised for wavebreaking and vertical mixing in earth's oceans is adapted to semiconvection, and the model is applied to actual stellar evolutions. The results obtained confirm that the Schwarzschild-Haerm (1958) criterion for semiconvection (i.e., marginal superadiabaticity) is essentially correct in cases where convective heat transport is adequate.
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