Speaker
Description
Since the middle of the last century, it has been known that the atmosphere of the Sun is orders of magnitudes hotter than its surface. Over the years, many studies have looked at the potential role of MHD waves in sustaining these high temperatures. Using 3D MHD simulations of transverse, Alfvenic waves, we look at the role of the complexity of the magnetic field and the power spectrum of the wave driver. We focus on the efficiency of the wave-based heating in our models, in particular whether heating provided by the waves can balance coronal losses. Using wave identifiers based on fundamental wave characteristics such as compressibility and direction of propagation we show that, for particular line(s)-of-sight and assumptions about the magnetic field, we can correctly identify properties of the Alfvén mode in synthetic observations of a transversely oscillating loop.
