3D simulations of strongly magnetic solar granulation reveal convective redshifts in absorption lines, originating from hot down-moving elements created by shocks and adiabatic compression in magnetically channeled flows.
K., et al.\ 2025, , 543, 1974
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Solar photospheric spectrum microvariability III. Radial velocities and line profiles in magnetic active-region granulation
3D simulations of strongly magnetic solar granulation reveal convective redshifts in absorption lines, originating from hot down-moving elements created by shocks and adiabatic compression in magnetically channeled flows.