The Solar and Stellar Coronae group employs spectroscopic, imaging, and stereoscopic techniques to analyse observations from extreme UV solar telescopes and coronagraphs. On the side of theory and (numerical) simulations we use magnetic modelling to extrapolate magnetic fields and 3D magneto-static and magneto-hydrodynamic models.
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Main goal of the group is to understand the structure, dynamics and heating of solar and stellar coronae. These outer atmospheres are heated to temperatures of more than a million degrees and show a large spatial and temporal variability.
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