heating of the solar atmosphere

The most important problem with our current solar model is the fact that the temperature  in  the chromosphere and corona increases with increasing distance from the core. The corona  reaches several million degrees higher than the photosphere, but it in the chromosphere where the larger electron density coupled with a few hundred degree rise in the temperature that the energy budget problem arises. This extra heating must be accounted for by in-situ heating (like a reconnection process in a solar flare) or energy carried by waves. The search for waves is only possible with high cadence datasets in multiple bandpasses. The work I carried out during my PhD involved looking for oscillatory signatures of waves in images sequences from ground- and space-based observatories.