On the large-scale dynamics and magnetic structure of solar active regions

Details On the large-scale dynamics and magnetic structure of solar active regions On the large-scale dynamics and magnetic structure of solar active regions

Dec 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...323..368k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 323, Dec. 1, 1987, p. 368-379.

Mathematics

Logic

42

Magnetic Field Configurations, Plasma Dynamics, Solar Activity, Solar Atmosphere, Solar Magnetic Field, Doppler Effect, Magnetic Signatures, Spatial Distribution, Stellar Spectrophotometry, Temporal Distribution

Scientific paper

The author has studied sets of carefully coaligned C IV Dopplergrams, photospheric magnetograms, and Hα filtergrams to infer the flow properties of active regions and the relationship of these flows to the active region magnetic fields. The combined data show that active regions can be naturally divided into three basic parts: strong field regions, weak field corridors between strong fields of opposite polarity, and surrounding weak field areas. An idealized topological model in which the vertical fields of strong field regions diverge very rapidly with height to become essentially horizontal in the adjacent low-lying areas is proposed. The picture is similar to canopy structures.

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