Statistics – Computation
Scientific paper
Mar 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..110..115s&link_type=abstract
(Solar Cycle Workshop, 1st, Pasadena, CA, Aug. 17-20, 1986) Solar Physics (ISSN 0038-0938), vol. 110, no. 1, 1987, p. 115-128.
Statistics
Computation
89
Coronal Loops, Polarity, Solar Activity, Solar Corona, Solar Magnetic Field, Sunspots, Buoyancy, Computational Astrophysics, Field Strength, Magnetic Flux
Scientific paper
A number of processes associated with the formation of active regions produce "U-loops": fluxtubes having two ends at the photosphere but otherwise still embedded in the convection zone. The mass trapped on the field lines of such loops makes them behave in a qualitative different way from the "omega-loops" that form active regions. It is shown that U-loops will disperse through the convection zone and form a weak (down to a few gauss) field that covers a significant fraction of the solar surface. This field is tentatively identified with the inner-network fields observed at Kitt Peak and Big Bear. The process by which these fields escape through the surface is described; a remarkable property is that it can make active regions fields apparently disappear in situ. The mixed polarity moving magnetic features near sunspots are interpreted as a locally intense form of this disappearance by escape of U-loops.
Spruit Hendrik C.
Title Alan M.
van Ballegooijen Adriaan A.
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