University Graz

The Sun is the only star where fine structures down to sizes below 100 km can be observed directly. Numerical simulations of the dynamics of the solar convection zone and the photosphere have shown that processes at these small scales (and even smaller) are essential to understand the complex phenomena of solar activity like sunspots, chromospheric heating, flares etc. This School, therefore, intends to provide the students an up-to-date knowledge on the following items: a) what are high-resolution solar observations, and how to overcome atmospheric turbulence; b) current and future instrumentation for high-resolution observations; c) high-resolution numerical simulation, their predictions, and interpretation; d) solar granulation and convection; e) dynamics of the photosphere; f) complexity of photospheric/chromospheric dynamics; g) comparison between numerical simulation and observations.