The vector structure of active magnetic fields

Details The vector structure of active magnetic fields The vector structure of active magnetic fields

May 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985svmf.nasa....7p&link_type=abstract

In NASA. Marshall Space Flight Center Meas. of Solar Vector Magnetic Fields p 7-16 (SEE N85-29869 18-92)

Mathematics

Magnetic Fields, Photosphere, Solar Atmosphere, Vectors (Mathematics), Gradients, Magnetic Properties, Maxwell Equation, Solar Physics, Sun, Vector Analysis

Scientific paper

Observations are needed to show the form of the strains introduced into the fields above the surface of the Sun. The longitudinal component alone does not provide the basic information, so that it has been necessary in the past to use the filamentary structure observed in Halpha to supplement the longitudinal information. Vector measurements provide the additional essential information to determine the strains, with the filamentary structure available as a check for consistency. It is to be expected, then, that vector measurements will permit a direct mapping of the strains imposed on the magnetic fields of active regions. It will be interesting to study the relation of those strains to the emergence of magnetic flux, flares, eruptive prominences, etc. In particular we may hope to study the relaxation of the strains via the dynamical nonequilibrium.

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