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The Coronal Power Spectrum from MHD Mode Conversion above Sunspots

  • Authors: Hemanthi Miriyala, Richard J. Morton, Elena Khomenko, Patrick Antolin, Gert J.J. Botha

Hemanthi Miriyala et al 2025 The Astrophysical Journal 979 .

  • Provider: AAS Journals

Caption: Figure 6.

Time evolutions of velocity projections of slow (left), fast (middle), and Alfvén (right) waves for a column of the simulation. The location in the domain is shown by the vertical line in Figure 5. The inclination angle and the azimuthal angles are (θϕ) = (30, 56) at the equipartition layer. The plots in the second row are similar but zoomed in to a vertical range of −1 Mm to 1 Mm for better clarity. The solid line is the equipartition layer and the region between the two dashed lines corresponds to the fast wave reflection region. The dotted line is the fast wave reflection region, which is estimated by taking the period Pn = Pc. All the velocity projections are scaled by a factor of ﹩\sqrt{{\rho }_{0}{c}_{s}}﹩ for the left panel and ﹩\sqrt{{\rho }_{0}{v}_{{\rm{A}}}}﹩ for the middle and right panels.

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