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A Statistical Study of Photospheric Magnetic Field Changes During 75 Solar Flares

  • Authors: J. S. Castellanos Durán, L. Kleint, and B. Calvo-Mozo

2018 The Astrophysical Journal 852 25.

  • Provider: AAS Journals

Caption: Figure 2.

HMI intensity images showing the flare sample, ordered by decreasing flare energy. Color-coded pixels indicate locations with ﹩{\rm{\Delta }}{B}_{\mathrm{LOS}}﹩, which are clipped at ±600 Mx cm−2 according to the color bar on the bottom. Blue axes and labels are used for flares where ﹩{\rm{\Delta }}{B}_{\mathrm{LOS}}﹩ were found. Red axes and labels represent flares without ﹩{\rm{\Delta }}{B}_{\mathrm{LOS}}﹩. Image scales are shown by the dashed bar with a length of 80″ in each image. Black boxes in the intensity images indicate the FoVs in Figure 4. Red stars denote the 18 flares that, in addition to classical stepwise changes, also showed other types of temporal evolutions of ﹩{B}_{\mathrm{LOS}}(t)﹩ (see Section 2.2).

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