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Progress in Earth and Planetary Science
Fig. 7 | Progress in Earth and Planetary Science

Fig. 7

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

Fig. 7

NLFFF for AR11158 at 00:00 UT on 15 February 2011 before a X2.2-class flare. a The B z distribution of the photospheric magnetic field, approximately 2 h before the occurrence of the X2.2-class flare observed by SDO/HMI. b Magnetic field lines from the NLFFF are superimposed on a; the format of the field lines is the same as in Fig. 6 d. The small inset corresponds to an enlarged view of the central area. c The magnetic twist distribution from Inoue et al. (2014a), where the vertical and horizontal axes are the twist and B z , respectively. The dashed line corresponds to T n = 1.0. The image is copyright AAS and reproduced by permission. d The magnetic field lines are plotted together with the surface corresponding to the critical height of the torus instability

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