Microwave emission is one of the most important sources of information about energetic electrons of non-thermal and hot thermal plasmas in solar flares. It is particularly valuable for observational diagnostics of flares in twisted coronal loops: while the polarisation can be used to evaluate the magnetic twist (Gordovskyy et al. 2017), loop oscillations, visible in microwave, can provide unique information about the magnetic relaxation and energy release process.
In this study, we use 3D MHD models of unstable twisted coronal loops (Gordovskyy et al. 2014) and the fast microwave code (Fleishman & Kuznetsov 2010) to investigate how the magnetic field evolution, as well as the dynamics of energetic electrons in the loop, affect intensity and circular polarisation of the microwave emission in the range 4-80 GHz. In particular, we investigate how the spatial distribution of circular polarisation, and the intensity and amplitude of the microwave oscillations change during the kink instability and the relaxation phases.