Speaker
Description
In this talk I will review recent progress and the remaining challenges in both modelling and analysing observed magnetohydrodynamic (MHD) waves in the lower solar atmosphere. To model waves in sunspot umbrae, we have had to go beyond the standard cylindrical flux tube model due to the irregular shapes of the MHD waveguides. For sunspots the umbra/penumbra boundary shape is reasonably static over the time scales of oscillations of interest. This makes solving the eigenvalue problem for MHD wave modes in sunspots tractable because of the assumption of time independent boundary shape conditions. However, the same cannot be said about pores that have highly dynamic boundary shape changes. I will highlight recent progress that has been made in this very challenging area of research.
| Sessions | Wave generation, energy transport, dissipation and heating |
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