The 3-d magnetic field structure of AR 6659 from a boundary element method solution under constant-α force-free field condition.

Details The 3-d magnetic field structure of AR 6659 from a boundary element method solution under constant-α force-free field condition. The 3-d magnetic field structure of AR 6659 from a boundary element method solution under constant-α force-free field condition.

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...298..277y&link_type=abstract

Astronomy and Astrophysics, v.298, p.277

Astronomy and Astrophysics

Astrophysics

23

Sun: Flares, Sun: Magnetic Fields, Mhd Methods: Numerical, Sun: Sunspots

Scientific paper

Using the boundary element method (BEM), the linear force-free magnetic field above the active region NOAA 6659 on 9 June, 1991 is reconstructed based on Huairou vector magnetograms with 180deg azimuth ambiguity removed. The associations of a 3B/X12 flare to the 3-D magnetic field structure are demonstrated. In particular, the following results are revealed by this study. (a) The 3B/X12 flare is probably due to the interaction between an energetic low-laid active magnetic loop along the magnetic neutral lines (thus revealing a highly sheared feature on the photosphere) and several other loops. (b) Each primary flare kernel seen from Hbeta_ image or white light, is located at foot-points of several interacting loops. (c) The currents flowing along the active low-laid loop deduced from the present computation are approximately 1x10^11^A, in an order consistent with that estimated from the high resolution observations. (d) The 3-d field distribution indicates that only a minor portion of magnetic field lines in the δ sunspot is connected locally and the majority of them are extended globally to the exterior of the region. This may explain the severe imbalance of magnetic flux between opposite polarities in great δ-sunspots. The present results support the idea that excess magnetic energy is probably suddenly released due to reconnection at separatrices by instability.

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