Magnetic shear. I - Hale region 16918

Details Magnetic shear. I - Hale region 16918 Magnetic shear. I - Hale region 16918

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...288..363a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 288, Jan. 1, 1985, p. 363-372.

Astronomy and Astrophysics

Astrophysics

35

Magnetohydrodynamics, Solar Flares, Solar Magnetic Field, Chromosphere, H Alpha Line, Lines Of Force, Shear, Solar Corona, Solar Maximum Mission, Solar Prominences, Solar Spectra

Scientific paper

Material motion observed in spectral lines of C IV, C II, and Ca II formed in the chromosphere-corona transition region and upper chromosphere exhibits patterns that are closely identified with magnetic field structure at photospheric levels. Assuming that the fluid flow follows magnetic lines of force, the authors use chromospheric and transition region Dopplergrams to infer the broad features of the magnetic field geometry in these upper layers. For Hale region 16918 they find an area in the transition region and upper chromosphere, centered roughly over the photospheric magnetic neutral line, in which the lines of force show a strong tendency to parallel the photospheric neutral line. The authors interpret this as evidence for magnetic shear, which is pronounced in the upper layers of the atmosphere.

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