SOLARNET Conference: The Many Scales of the Magnetic Sun

We have exploited seeing-free and high-quality observations of several small magnetic pores from the High Resolution Telescope (HRT) of the Polarimetric and Helioseismic Imager (PHI) on board the Solar Orbiter spacecraft, during its first close perihelion in March 2022 (at a distance of 0.5 au from the Sun). Only such small magnetic pores, captured at stable observing conditions, could manifest (large) area fluctuations, on the order of 30% variations, that is an indication of (non-linear) fast sausage (surface) modes. Furthermore, cross correlations between perturbations in intensity, area, line-of-sight velocity, and magnetic fields have provided us with additional wave signatures, that together with applications of modern analysis techniques, such as the Spectral Proper Orthogonal Decomposition (SPOD), we have been able to characterise the underlying MHD wave modes in more details.