Programme by Session

We present a family of multi-layered asymmetric waveguide models as a generalisation of the classical (symmetric) slab configuration and demonstrate their wide range of applications using high-resolution solar observations.
Diagnosing the solar atmospheric plasma is one of the major challenges in solar physics. Magnetohydrodynamic (MHD) waves, by means of applying the methods of solar magneto-seismology (SMS), provide a powerful tool to diagnose the solar plasma in a range of MHD waveguides e.g. from small magnetic bright points (MBPs), pores to large structures like prominences. Here, we present the framework of a new model to describe MHD wave propagation. Namely, we employ a family of asymmetric Cartesian waveguide models that can better capture the structured solar atmosphere. We describe a general multi-layered, stationary MHD waveguide and its asymmetric (externally magnetic and non-magnetic) one-slab special cases. Additionally, we investigate the effect of one or more steady bulk flows on the dispersion and stability of MHD waves in an asymmetric magnetic slab system.
With the recent and ongoing developments in high-resolution solar observations, each of these models can be utilised to describe different features in the solar atmosphere, such as elongated MBPs, light walls, fibrils, prominences, and CME flanks. We show a sample of these applications and demonstrate how the SMS diagnostic power of waveguide asymmetry can be utilised in these structures.