# COMMUNICATIONS / MITTEILUNGEN

## I.K. Csada

## On the Theory of Rotating Magnetic Stars II

No. 37
Budapest, 1955

## Abstract

The basic equations of a rotating magnetic star are given in the preceding paper.
In the present one the approximate solutions of these equations are sought for under
very general conditions. No idealized structure is assumed for producing either the
velocity field or the magnetic field. So, besides axial rotation, meridional motions too
are examined, and the vector of the magnetic field strength is supposed not only as
locating itself in the plane of the meridian, but also as having a component perpendicular
to it. This component forms the so-called toroidal magnetic field, whose mathematical
investigation explained in the present paper finds itself among the first articles on
such a subject.
Whereas the first four parts of this paper contain the pure mathematical dis-
cussion of the problem, from the fifth part on the results of the theory are compared
with the different solar and astrophysical observations. The theory gives the laws
of the distribution of the angular velocity. on the solar surface and those of meridional
motion correctly. It follows from the theory that the viscosity of the solar matter must
be very great, the electric conductivity very small. These results are in harmony with
the proprieties guessed till now of hydromagnetical turbulence.
On the ground of the theory an external magnetic dipole field cannot be deduced
for the Sun. In accordance with the theory the external field has an octopole structure.
From the results it may be concluded that the velocity distribution of the typical mag-
netic stars cannot be such as that of the Sun, because it is very improbable that the
powerful magnetic fields of the stars would arise from a field having a pole of higher
order.
A relation between the radius of the star and its viscosity coefficient can be
established. The correctness of this relation is examined by the aid of data of pertinent
literature.
ADS

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