Solar prominence model based on eigenvalue solutions. II - Filaments in the vertical magnetic fields

Details Solar prominence model based on eigenvalue solutions. II - Filaments in the vertical magnetic fields Solar prominence model based on eigenvalue solutions. II - Filaments in the vertical magnetic fields

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...336.1041o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 336, Jan. 15, 1989, p. 1041-1049.

Astronomy and Astrophysics

Astrophysics

5

Eigenvalues, Solar Magnetic Field, Solar Prominences, Two Dimensional Models, Density Distribution, Plasma Density, Solar Atmosphere, Vertical Distribution

Scientific paper

An eigenvalue approach is employed to study the equilibrium of a solar filament in a stratified atmosphere with a vertical magnetic field. It is shown that the external vertical magnetic field can redistribute plasma density and create the positive density excess or negative density excess (cavity) above the prominence, depending on the relative width and the relative strength of the filament's magnetic field.

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