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On the Nature of the Photospheric Horizontal Magnetic Field Increase in Major Solar Flares

  • Authors: Lijuan Liu, Zhenjun Zhou, Yuming Wang, Xudong Sun, Guoqiang Wang

Lijuan Liu et al 2022 The Astrophysical Journal Letters 934 .

  • Provider: AAS Journals

Caption: Figure 1.

Evolution of B h increase (abbreviated as “B h I” in figures) in case 33. (a) A postflare B h difference image. The black-green contours outline the postflare mask of the B h increase (pixel value ≥ 120 G); the black contours outline the flare ribbons at one moment for comparison. “t” (in minutes) indicates time after flare start (GOES start time). S p and S n are slices in positive and negative polarities used to determine the representative points of the region fronts (cyan squares). (b)–(c) Spatiotemporal evolution masks for the B h increase and flare ribbons, color-coded by the time elapsed from flare start. Colored contours in (c) outline B h -increase regions at different times. The associated animation lasts from 2017-09-06T17:38 to 2017-09-06T18:56, showing the B h increase and ribbon evolution. Its frames have a similar layout to the figure.

(An animation of this figure is available.)

The video/animation of this figure is available in the online journal.

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