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Ian Lerche
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Journal of Physics and Astronomy Research

Some Notes on Self-similar Axisymmetric Force-free Magnetic Fields and Rotating Magnetospheres

Ian Lerche

Institute of Earth Sciences, Faculty of Natural Sciences III, Martin-Luther University of Halle, Germany

Distinguished Professor Emeritus; Email: lercheian@yahoo.com

Accepted 25 September, 2014.

Citation: Lerche I (2014). Some Notes on Self-similar Axisymmetric Force-free Magnetic Fields and Rotating Magnetospheres. Journal of Physics and Astronomy Research 1(2): 007-012.



Copyright: © 2014 Lerche I. This is an open-access article distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are cited.

Abstract

An axisymmetric force-free magnetic field in spherical coordinates has a relationship between its azimuthal component to its poloidal flux-function. A power law dependence for the connection admits separable field solutions but poses a nonlinear eigenvalue boundary-value problem for the separation parameter (Low and Lou, Astrophys. J. 352, 343 (1990)).When the atmosphere of a star is rotating the problem complexity increases. These Notes consider the nonlinear eigenvalue spectrum, providing an understanding of the eigen functions and relationship between the field's degree of multi-polarity, the rotation and rate of radial decay as illustrated through a polytropic equation of state. The Notes are restricted to uniform rotation and to axisymmetric fields. Dominant effects are presented of rotation in changing the spatial patterns of the magnetic field from those without rotation. For differential rotation and non-axisymmetric force-free fields there may be field solutions of even richer topological structure but the governing equations have remained intractable to date. Perhaps the methods and discussion given here for the uniformly rotating situation indicate a possible procedure for such problems that need to be solved urgently for a more complete understanding of force-free magnetic fields in stellar atmospheres.

Key words: Rotating stellar atmospheres, axisymmetric magnetic fields, polytropes, nonlinear, eigenvalue equations