Programme by Session

Closing the gap between observations and numerical models is a critical step in helping us to identify the mechanism(s) responsible for coronal heating. Through the use of forward modelling, we can transform the model results into synthetic emission data, allowing us to compare models and observations in a meaningful way. We present the results of numerical simulations investigating the braiding of two coronal magnetic flux tubes. Using forward modelling, we infer if there are any observational signatures associated with this particular model’s heating mechanisms. We discuss the evolution of synthetic intensities and Doppler velocities in order to predict observables which would highlight the existence of such processes in the Sun’s atmosphere. Analysing such results from multiple heating models will allow us to identify characteristics of energy release in the solar corona.