Coronal loops and active region structure

Details Coronal loops and active region structure Coronal loops and active region structure

Jan 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981soph...69...99w&link_type=abstract

Solar Physics, vol. 69, Jan. 1981, p. 99-118.

Astronomy and Astrophysics

Astronomy

37

Coronal Loops, Magnetic Field Configurations, Solar Activity, Solar Magnetic Field, Solar Physics, Calcium, H Alpha Line, K Lines, Potassium, Skylab Program, Solar Flux, X Ray Astronomy

Scientific paper

Synoptic H-alpha Ca K, magnetograph and Skylab soft X-ray and EUV data were compared for the purpose of identifying the basic coronal magnetic structure of loops in a 'typical' active region and studying its evolution. A complex of activity in July 1973, especially McMath 12417, was emphasized. The principal results are: (1) most of the brightest loops connected the bright f plage to either the sunspot penumbra or to p satellite spots; no non-flaring X-ray loops end in umbrae; (2) short, bright loops had one or both ends in regions of emergent flux, strong field or high field gradients; (3) stable, strongly sheared loop arcades formed over filaments; (4) EFRs were always associated with compact X-ray arcades; and (5) loops connecting to other active regions had their bases in outlying plage of weak field strength in McM 417 where H-alpha fibrils marked the direction of the loops

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