Studying the thermodynamics of coronal jets through modeling- and observational diagnostics techniques

We present a comprehensive study of simulated and observed coronal jets using EUV and soft X-ray narrow-band images and EUV high resolution spectra. The goal of our study is to understand the thermodynamics and time evolution of jets and their impact on the coronal plasma. We simulate jets with a full 3D MHD coronal model with separate electron and proton temperatures and heating due to Alfvén wave turbulence. Due to the fast dynamics of the small-scale eruptive reconnections at the footpoint of the jet, it is essential to undertake this effort with a model with separate electron and proton temperatures to interpret the observed signatures in EUV and soft X-ray bands. The obtained synthetic images are compared to observations done by the instrumentations of SDO, STEREO and Hinode space crafts. The turbulence in this model is ideally suited to analyze the spectroscopic signatures, such as line broadening. The 3-hour long simulation of jets interacting with the global solar corona shows plasma responses potentially being observed with the upcoming Solar Probe Plus mission.