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Magnetic Prandtl Number and Astrophysical Convection

Published online by Cambridge University Press:  25 April 2016

J. O. Murphy  and
J. M. Lopez
J. O. Murphy
Affiliation:
Department of Mathematics, Monash University
J. M. Lopez
Affiliation:
Department of Mathematics, Monash University
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Extract

In the astrophysical context, where the effects of a magnetic field on stellar convective processes have to be taken into account, we have ϰ > > η > > ν (Weiss 1977) where ϰ, η and ν are respectively the thermal, magnetic and viscous diffusivities.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 4 , Issue 2 , 1981 , pp. 208 - 209
Copyright
Copyright © Astronomical Society of Australia 1981

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References

Chandrasekhar, S., ‘ Hydrodynamic and Hydromagnetic Stability ’, Oxford University Press (1961).Google Scholar
Weiss, N. O., Problems in Stellar Convection, I.A.U. Colloquium No. 38, 176 (1976).Google Scholar
Van der Borght, R., and Murphy, J. O., Aust. J. Phys., 26, 617 (1973).CrossRefGoogle Scholar