MUSE EUV spectroscopy of a coronal loop system undergoing MHD-avalanche

Solar magnetic field dynamics is driven by turbulent photospheric movements, leading to the twisting and tangling of magnetic field lines in the corona. As a consequence, magnetic stresses continually accumulate. In this environment, twisted magnetic flux tubes can become susceptible to kink instability, resulting in the release of magnetic energy through sudden, widespread heating events. Recent research has unveiled that this kink instability can spread to adjacent flux tubes, triggering an avalanche process that involves larger-scale coronal loops. The initial helical current sheet progressively disintegrates in a turbulent manner, forming smaller-scale sheets. These turbulent processes give rise to a series of irregular heat pulses, akin to nanoflare storms. These magnetic phenomena are highly dynamic and nonlinear, demanding modeling through time-dependent 3D magnetohydrodynamic simulations, often necessitating high-performance computing systems. To make meaningful predictions that can be compared with solar observations, two critical advancements are essential. First, the modeling approach must encompass all crucial physical components, including a comprehensive representation of the plasma atmosphere, to derive realistic observational outcomes. Second, observational techniques must achieve sufficient temporal and spatial resolution within the pertinent spectral bands. In their 2023 study, Cozzo et al. provide a detailed 3D magnetohydrodynamic (MHD) model that enables the derivation of observable parameters in the extreme ultraviolet (EUV) band. The EUV spectrometer designed for the upcoming MUSE mission is specifically designed to explore plasma structure and dynamics at sub-arcsecond resolution, with sampling rates as short as a few seconds. In this research, we present preliminary EUV diagnostic results obtained from our model, tailored for the MUSE mission, to shed light on the MHD-avalanche scenario.