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Energetics and Emission in a Simulated Solar Flare Initialized by a Non-force-free Magnetic Field

  • Authors: W. Bate, M. Gordovskyy, A. Prasad, A. S. Brun, A. Strugarek, M. V. Sieyra, P. K. Browning, S. Inoue, K. Matsumoto, A. Roddanavar

W. Bate et al 2026 The Astrophysical Journal 1006 .

  • Provider: AAS Journals

Caption: Figure 3.

Magnetic field restructuring in the two simulations. The left column shows the NLFF case, and the right column shows the non-force-free case. All panels correspond to the same times, with field line connectivity compared between t = 0 and t = 100tA. The rows show different viewing angles: isometric and projections along the x-, y-, and z-axes. Red field lines indicate structures that are initially closed at t = 0, while the corresponding purple lines show their connectivity at t = 100tA, highlighting field lines that become open. Blue field lines denote structures at t = 0 whose footpoints undergo significant displacement (>5 Mm), with their later positions shown in green at t = 100tA.

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