Observational Signatures of Waves and Flows in the Solar Corona

TL;DR

This study uses forward-modeling to identify observational signatures that distinguish slow magneto-acoustic waves from quasi-periodic flows in the solar corona, highlighting the ratio of Doppler velocity mean to amplitude as a key indicator.

Contribution

The paper introduces a forward-modeling approach to differentiate between wave and flow signatures in coronal observations, emphasizing the robustness of the Doppler velocity ratio as a diagnostic tool.

Findings

The ratio of mean to amplitude of Doppler velocity exceeds one for flows.

Rapid change in line widths with line-of-sight angle is characteristic of waves.

Flow models show a higher line width to Doppler velocity amplitude ratio.

Abstract

Propagating perturbations have been observed in extended coronal loop structures for a number of years, but the interpretation in terms of slow (propagating) magneto-acoustic waves and/or as quasi-periodic upflows remains unresolved. We used forward-modelling to construct observational signatures associated with a simple slow magneto-acoustic wave or periodic flow model. Observational signatures were computed for the 171 {\AA} Fe ix and the 193 {\AA} Fe xii spectral lines. Although there are many differences between the flow and wave models, we did not find any clear, robust observational characteristics that can be used in isolation ( i.e. that do not rely on a comparison between the models). For the waves model, a relatively rapid change of the average line widths as a function of (shallow) line-of-sight angles was found, whereas the ratio of the line width amplitudes to the Doppler velocity amplitudes is relatively high for the flow model. The most robust observational signature found is that the ratio of the mean to the amplitudes of the Doppler velocity is always higher than one for the flow model. This ratio is substantially higher for flows than for waves, and for the flows model used in the study is exactly the same in the 171 {\AA} Fe ix and the 193 {\AA} Fe xii spectral lines. However, these potential observational signatures need to be treated cautiously because they are likely to be model-dependent.