Spectroscopic indication of suprathermal ions in the solar corona

Using spectroscopic data, we support the possibility of suprathermal distributions of coronal ions by fitting the equivalent kappa functions to their emission line profiles. We fit different kappa and Gaussian model functions to line profiles of the strong Fe xv line at 284.16 Angstroms, across two large-field spectroscopic rasters taken in a solar active region. Both single- and double-component Gaussian models are applied, as well as two kappa models, one with a free width parameter allowing for and the other with a constrained width that precludes "microturbulence". We then compare the goodness of fit of the computed best fits for each model. The kappa distribution is a generalization, or superset, of the Maxwellian, so they are able to fit line profiles more precisely than a Gaussian. In most of the data, the best-fit kappa model produces much lower residuals across the profile than any single Gaussian and sometimes double Gaussian. Most importantly, the distribution of estimated kappa values is found to lie mostly in the low-kappa range, implying ion populations far from Maxwellian. Even when the width is removed as a free parameter of fit, the kappa model is still able to fit the data credibly, again with low best-fit values of kappa. We find the shape of the Fe xv line, in the vast majority of the data analyzed, to be indicative of a highly suprathermal ion population.