The magnetic and velocity structure adjacent to solar active regions

Details The magnetic and velocity structure adjacent to solar active regions The magnetic and velocity structure adjacent to solar active regions

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...318..437a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 318, July 1, 1987, p. 437-444.

Astronomy and Astrophysics

Astrophysics

10

Kinetic Energy, Solar Atmosphere, Solar Flares, Solar Magnetic Field, Ultraviolet Spectra, Flow Distribution, H Alpha Line, Line Of Sight, Velocity Distribution

Scientific paper

Results from a number of earlier papers relating velocity patterns observed in the C IV line at 154.8 nm to photospheric magnetic-field patterns are combined to develop a qualitative model of the magnetic-field geometry outside of the strong field areas of active regions. The motion is assumed to originate at the crests of magnetic arcades and flow downward along field lines, which are assumed to be elliptical in shape with the major axis in the photosphere. It is found that the ratio of the major axis to the minor axis of the ellipse must be less than two for fields under 100 G. Also, it is concluded that the magnetic neutral surfaces defined by the loci of horizontal field lines are often tilted at a large angle to the vertical at the altitude of the C IV emission.

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