MUSE EUV spectroscopy of a kink-unstable coronal loop system

Turbulent photospheric motions drive the solar magnetic field to twist and tangle, making magnetic stresses continuously grow in the corona. Thin magnetic flux tubes can become kink-unstable and magnetic energy can be released through impulsive and widespread heating events. It has been recently established that the kink-instability can propagate to nearby flux tubes and determine an avalanche process to involve larger scale coronal loops. The initial helical current sheet progressively fragments in a turbulent way into smaller scale sheets. Their turbulent dissipation leads to a sequence of a-periodic heat pulses, similar to nanoflare storms. These magnetic processes are highly dynamic and non linear, and can be modelled with time-dependent 3D magnetohydrodynamic simulations on high performance computing systems. Predictions to compare with solar observations require advances on two fronts. The modeling must include all important physical ingredients and a complete plasma atmosphere to derive realistic observables. The observations must resolve into sufficiently small temporal and spatial scales in the relevant spectral bands. Cozzo et al. (2023) describe a detailed 3D MHD model which allows for the derivation of observables in the EUV band. The EUV spectrometer on the forth-coming MUSE mission is tailored for probing plasma structure and dynamics at sub-arcsecond resolution with sampling rates of few seconds. In this work we show preliminary EUV diagnostics of the scenario obtained from our model for the MUSE mission.