Depth of origin of solar active regions

Details Depth of origin of solar active regions Depth of origin of solar active regions

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...280..423p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 280, May 1, 1984, p. 423-427.

Other

28

Magnetohydrodynamics, Solar Activity, Solar Magnetic Field, Electrical Resistivity, Magnetic Flux, Photosphere, Sunspots

Scientific paper

Observations show that the individual bipolar magnetic regions on the sun remain confined during their decay phase, with much of the magnetic field pulling back under the surface, in reverse of the earlier emergence. This suggests that the magnetic field is held on a short rein by subsurface forces, for otherwise the region would decay entirely by dispersing across the face of the sun. With the simple assumption that the fields at the surface are controlled from well-defined anchor points at a depth h, it is possible to relate the length l of the bipolar region at the surface to the depth h, with h about equal to l. The observed dimensions l about equal to 100,000 km for normal active regions, and l about equal to 10,000 km for the ephemeral active regions, indicate comparable depths of origin. More detailed observational studies of the active regions may be expected to shed further light on the problem.

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