Solar magnetic fields and convection. IV - Magnetic flux ropes and their fibres

Details Solar magnetic fields and convection. IV - Magnetic flux ropes and their fibres Solar magnetic fields and convection. IV - Magnetic flux ropes and their fibres

Mar 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976ap%26ss..40...73p&link_type=abstract

Astrophysics and Space Science, vol. 40, Mar. 1976, p. 73-90.

Astronomy and Astrophysics

Astrophysics

11

Lines Of Force, Magnetic Field Configurations, Magnetic Flux, Solar Magnetic Field, Dynamo Theory, Magnetic Effects, Stellar Models, Sunspots

Scientific paper

The flux-rope theory of solar magnetic fields is based on the concept of a toroidal flux created by differential rotation and simultaneously rolled into helically twisted ropes which later emerge as inverted U's to produce active regions. This theory is further developed by taking account of additional observational data. Evidence is presented to show that sunspot magnetic fields are helically twisted, that all solar fields are fibrous, and that these fibers are twisted. Based on this evidence, it is concluded that (1) sunspot magnetic fields are in the form of helically twisted flux ropes which were already twisted before they emerged as inverted U structures, and (2) all solar magnetic fields are made up of individual flux fibers which may be twisted into bunches that are, in turn, twisted together to form flux ropes. The kinematics of flux fibers and ropes is discussed, the formation of a sunspot is explained in terms of the upward motion of a frayed flux rope, and sunspot decay is shown to occur when the outer layer of fibers unwinds. A model for sunspot dynamics is developed which can explain the observed radial decrease in magnetic-field strength, umbral flashes, the umbral boundary, and the sunspot energy deficit. It is concluded that the dynamo, diffuse-field, and other convective models of solar magnetic fields are inconsistent with the observational data.

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