Physics
Scientific paper
Aug 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982soph...79..267g&link_type=abstract
Solar Physics, vol. 79, Aug. 1982, p. 267-278.
Physics
84
Magnetic Field Configurations, Magnetic Signatures, Photosphere, Solar Activity, Solar Atmosphere, Solar Magnetic Field, Magnetic Flux, Penumbras, Solar Spectra, Sunspots
Scientific paper
The magnetic field above two unrelated active regions on September 11-12, 1974 has been studied by means of magnetograms obtained in C I 9111, Fe I 8688, Ca II 8542, and H-alpha. In C I, originating low in the photosphere, the fields are strong and sharply defined, by contrast with Ca II and H-alpha, where they are very diffuse. The similar diffuseness of Fe I is due to the spreading of the field with height to form nearly horizontal magnetic canopies over regions free of field at lower levels. Within a region between two small sunspots some 140 Mm apart, the canopy height is typically 300-400 km, and it is about 150-250 km within a small superpenumbra. It is hypothesized that the chromospheric fibrils taken to delineate the field configuration are not due primarily to lateral variations in field, but rather to differences in density or excitation of gas across the lines of force.
Giovanelli R. G.
Jones Philip H.
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