Evolution of twisted magnetic fields

Details Evolution of twisted magnetic fields Evolution of twisted magnetic fields

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...295..642z&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 295, Aug. 15, 1985, p. 642-647.

Astronomy and Astrophysics

Astrophysics

38

Magnetic Field Configurations, Magnetic Flux, Magnetohydrodynamic Stability, Photosphere, Solar Corona, Solar Magnetic Field, Cartesian Coordinates, Differential Equations, Euler Equations Of Motion, Integral Equations, Topology

Scientific paper

The magnetic field of the solar corona evolves quasi-statically in response to slowly changing photospheric boundary conditions. The magnetic topology is preserved by the low resistivity of the solar atmosphere. It is shown that a magnetic flux coordinate system simplifies the problem of calculating field evolution with invariant topology. As an example, the equilibrium of a thin magnetic flux tube with small twist per unit length is calculated.

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