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Flare Reconnection-driven Magnetic Field and Lorentz Force Variations at the Sun’s Surface

  • Authors: Krzysztof Barczynski, Guillaume Aulanier, Sophie Masson, and Michael S. Wheatland

2019 The Astrophysical Journal 877 67.

  • Provider: AAS Journals

Caption: Figure 3.

Vertical component of the current density ﹩{j}_{z}(z=0.1)﹩ at three different times during the eruption. The negative and positive currents are defined by the blue and red color scale. Arrows represent magnetic field components ﹩{B}_{x}(z=0.1)﹩ and ﹩{B}_{y}(z=0.1)﹩. The black contours indicate the vertical component of the magnetic field ﹩{B}_{z}(z=0.1)=-1﹩ and ﹩{B}_{z}(z=0.1)=1﹩. The color-coded boxes (0–9) mark regions that are used in the further analysis. The animation begins at ﹩t=164{t}_{A}﹩ and ends at ﹩t=244{t}_{A}﹩.

(An animation of this figure is available.)

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

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