Description
Coronal loops are the basic structures of the solar corona resulting from the confinement of the multi-thermal coronal plasma in magnetic flux tubes.
Improving their modeling could help in understanding the physical processes involved in the formation and evolution of loops, and the mechanisms of energy transfer in the solar atmosphere.
In this work we performed several direct numerical simulations of a coronal loop by integrating the compressible 3D MagnetoHydroDynamics (MHD) using a pseudo-spectral code. Equations are solved in a triply periodic elongated box in which we evolve an initial condition given by a turbulent plasma flow perturbed with torsional Alfvén waves.
We explore a parameter space compatible with the observations and investigate how the interaction between turbulence and waves affects the dynamics of the system. Finally, we compute the spectral moments (i.e. line intensity, Doppler velocity) integrated along the line of sight to mimic the future observations of the corona with the MUlti-Slit Explorer (MUSE).
We study the spectra of physical observables from the synthetic data (e.g., intensity , Doppler shift velocities, etc) and relate them to the spectra of the plasma parameters (density, velocity, temperature fields) from the 3D simulations.
