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Two-dimensional Radiative Magnetohydrodynamic Simulations of Partial Ionization in the Chromosphere. II. Dynamics and Energetics of the Low Solar Atmosphere

  • Authors: Juan Martínez-Sykora, Bart De Pontieu, Mats Carlsson, Viggo H. Hansteen, Daniel Nóbrega-Siverio, and Boris V. Gudiksen

2017 The Astrophysical Journal 847 36.

  • Provider: AAS Journals

Caption: Figure 13.

Top row: maps of the temperature with white magnetic field lines (panel (a)), density (panel (d)), divergence of velocity, with velocity vectors in white (panel (g)), the horizontal magnetic field strength (panel (j)), and the electric current density perpendicular to the plane of the simulation (panel (m)) for the non-GOL simulation at t = 1690 s (snapshot = 376). Middle row: same, but for the GOL simulation at t = 1460 s (snapshot = 352), with, respectively, panels (b), (e), (h), (k) and (n). Bottom row: Joule heating from the ambipolar diffusion (panel (c)), the ambipolar diffusion (panel (f)), and the vertical Poynting flux due to the vertical (panel (i)) and horizontal (panel (l)) ambipolar velocity for the GOL simulation. The white contours correspond to a 4000 K temperature. The region shown is x = [50, 57] Mm and x = [15, 22] Mm for the non-GOL and GOL simulations, respectively.

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