New light on an old problem of the cores of solar resonance lines

We examine data and calculations for the resonance lines of Hi, Mgii, and Caii, the self-reversed cores of which form in the upper chromosphere. Based on 3D simulations, as well as data for the Mgiilines from the Interface Region Imaging Spectrograph (IRIS), we argue that the resolution lies not in velocity fields on scales in either of the micro- or macroturbulent limits.

Macroturbulence is ruled out using observations of optically thin lines formed in the upper chromosphere, and by showing that it would need to have unreasonably special properties to account for critical observations of the Mgiiresonance lines from the IRIS mission. The power in "turbulence" in the upper chromosphere may therefore be substantially lower than earlier analyses have inferred. Instead, in 3D calculations horizontal radiative transfer produces smoother source functions, smoothing out intensity gradients in wavelength and in space.