Magnetic field of a flare flux

Details Magnetic field of a flare flux Magnetic field of a flare flux

Feb 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977izssr..41q.242p&link_type=abstract

(Mezhdunarodnyi Seminar po Aktivnym Protsessam na Solntse i Probleme Solnechnykh Neitrino, 8th, Leningrad, USSR, Sept. 25-27, 19

Astronomy and Astrophysics

Astronomy

Astronomical Models, Solar Flares, Solar Magnetic Field, Solar Wind, Interplanetary Magnetic Fields, Lines Of Force, Magnetic Field Configurations, Magnetic Flux, Satellite Observation

Scientific paper

Theoretical models and experimental data on the structure of the mass flux ejected in a solar flare and the magnetic field trapped within that flux are reviewed. Data obtained by earth satellites are used to evaluate parameters of a flare flux at heliocentric distances of about 1 AU and to examine near-earth variations in plasma parameters due to piston-type waves behind the interplanetary shock front. Based on comparisons between the theoretical models and experimental data, it is concluded that: (1) a flare flux, or at least its leading portion, can be divided into four regions, one containing the unperturbed solar-wind magnetic field, one containing the compressed solar-wind field, and two containing the intrinsic field of the flux; (2) the vertical component of the flux field possesses a regular variable constituent; (3) the lines of force of the vertical field are generally closed; and (4) the regular constituent of the vertical field is governed by the large-scale magnetic field in the flare region on the sun.

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