An evolutionary feature of the magnetic field related to flares in active regions

Astronomy and Astrophysics – Astronomy

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Magnetic Field Configurations, Magnetic Field Inversions, Magnetic Field Reconnection, Magnetic Flux, Photosphere, Polarity, Solar Activity, Solar Flares, Solar Magnetic Field, Solar X-Rays, Sunspots, X Ray Astronomy, Convective Flow, Gradients, H Alpha Line, Magnetic Signatures, Mass Flow, Umbras

Scientific paper

An evolutionary feature of the magnetic field related to flares in active regions - Incorporation of the Magnetic Flux of the Same Polarity (IMFSP) was studied in this paper. The statistics show that IMFSP related to a major X-ray flare (I greater than or equal to M) needs to have a stronger magnetic strength and gradient: (1) Two or more magnetic fluxes of the same polarity located near a magnetic area of the opposite polarity split or push away the flux of the opposite polarity and merge together. The maximum magnetic strength among them is not less than 320 G, and the minimum magnetic strength is not less than 80 G. (2) The new polarity inversion line is formed after the merger. The maximum gradient of the longitudinal field near the new polarity inversion line is not less than 0.12 G/km. The statistics also show that IMFSP is a rare phenomenon, 92% of them are accompanied by major X-flares. IMFSP is unlikely induced by two effects at least: (1) the horizontal motion of the matter beneath the photospheric surface moves the magnetic flux; (2) the magnetic flux emerges and grows continuously. The physical reasons that IMFSP results in the flare are discussed.

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