Physics
Scientific paper
Dec 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..136..269z&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 136, Dec. 1991, p. 269-293. Research supported by Chinese Academy of Sciences, NNSFC, and M
Physics
24
Chromosphere, Fine Structure, Mass Flow, Photosphere, Solar Activity, Solar Magnetic Field, H Alpha Line, H Beta Line, Line Spectra, Magnetic Field Configurations
Scientific paper
The relations between photospheric vector magnetic fields, chromospheric longitudinal magnetic fields and velocity fields in a solar active region are analyzed. Agreements between the photospheric and chromospheric magnetograms can be found in large-scale structures or in the stronger magnetic structures, but differences also can be found in the fine structures or in other places, which reflect the variation of the magnetic force lines from the photosphere to the chromosphere. The chromospheric superpenumbral magnetic field, measured by the H-beta line, presents a spokelike structure. It consists of thick magnetic fibrils which are different from photospheric penumbral magnetic fibrils. The outer superpenumbral magnetic field is almost horizontal. The direction of the chromospheric magnetic fibrils is generally parallel to the transverse components of the photospheric vector magnetic fields.
Ai Guoxiang
Kurokawa Hiroki
Sakurai Takashi
Zhang Hongqi
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