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Fig. 6 | Progress in Earth and Planetary Science

Fig. 6

From: Magnetohydrodynamics modeling of coronal magnetic field and solar eruptions based on the photospheric magnetic field

Fig. 6

NLFFF for AR11158 at 16:00 UT on 13 February 2011 before a M6.6-class flare. a Photospheric magnetic field obtained by SDO/HMI, 90 min before the M6.6-class flare, with the B z distribution plotted in red and blue. b The two panels show enlarged views of the central area in a; they show the B z distribution and the horizontal fields with arrows, with the PIL in black. The upper and lower panels show the horizontal fields of the potential field and the observed fields, respectively. c The potential field (in green) is superimposed on the data in a. d The NLFFF based on the MHD relaxation method (Inoue et al. 2014b) is plotted as in c, except that the strength of the current density is mapped onto the field line. e EUV images observed at 171 Å from the SDO/AIA at 16:00 UT on 13 February 2011. f The field lines, in the same format as in d, are superimposed on (e)

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