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Magnetic Fields in Slowly Rotating Stars

Published online by Cambridge University Press:  25 April 2016

G.F. Davies
G.F. Davies*
Affiliation:
Mathematics Department, Monash University, Melbourne
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Extract

Those solutions which have so far been obtained to the problem of a star with both rotation and a magnetic field have been for certain special cases, mostly time-independent. It is known that, except for stars with special rotation laws, a rotating star in hydrostatic equilibrium cannot maintain thermal equilibrium without generating slow meridional circulation of matter. It is also known that an axially symmetric field with no azimuthal component tends very strongly to keep the star in a state of isorotation, with the angular velocity constant along field lines. A magnetic field also tends to upset thermal equilibrium and produce meridional circulation. In the absence of rotation, an equilibrium poloidal field has recently been found for which there is no circulation. The present paper reports analogous equilibrium solutions for a star which is in uniform rotation.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 1 , Issue 3 , February 1968 , pp. 89
Copyright
Copyright © Astronomical Society of Australia 1968

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References

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