Shifting and broadening of coronal spectral lines by nanoflare heating

The heating of the solar corona by nanoflares is one of the most succesful theories in recent times to explain the wide variety of available observations. In a recent work we developed and analyzed a model based on coronal loops formed by elemental magnetic strands that interact with each other, reconnecting and consequently heating the plasma. Each of these heating events (or cluster of linked events) is considered a nanoflare. In a later article we showed that the model reproduces the main statistical characteristics of observed coronal loop lightcurves and the typical emission measure distributions obtained from observations. One of the predictions of the model is the presence of intense plasma flows in the heated strands. The summed radiative emission of strands at different temperatures and velocities produce spectral lines of coronal ions with characteristic broadenings and Doppler shifts. In this work, we study the contribution to emission of flows with different temperatures and velocities obtained with our model and construct synthetic spectral lines that we plan to compare in the future with observational results.