Chatzistergos, T.; Ermolli, I.; Krivova, N. A.; Solanki, S. K.; Banerjee, D.; Barata, T.; Belik, M.; Gafeira, R.; Garcia, A.; Hanaoka, Y.et al.; Hegde, M.; Klimeš, J.; Korokhin, V. V.; Lourenço, A.; Malherbe, J.-M.; Marchenko, G. P.; Peixinho, N.; Sakurai, T.; Tlatov, A. G.: Analysis of full-disc Ca II K spectroheliograms III. Plage area composite series covering 1892–2019. Astronomy and Astrophysics 639, A88 (2020)
Guglielmino, S. L.; Pillet, V. M.; Cobo, B. R.; Rubio, L. R. B.; Iniesta, J. C. d. T.; Solanki, S. K.; Riethmüller, T.; Zuccarello, F.: On the Magnetic Nature of an Exploding Granule as Revealed by Sunrise/IMaX. The Astrophysical Journal 896 (1), 62 (2020)
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.
Our research focusses on ultraviolet imaging and spectroscopy techniques, targeting at solar coronal features with a variety of scientific topics and methods that include (among other things) morphology and dynamics of coronal holes, spicules, sunspots, prominences/filaments and plumes, coronal heating, jets, flares, solar wind acceleration, density and temperature diagnostic, abundances and line identification.
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.
STEREO ist eine Mission der NASA, die erstmalig 3D-Beobachtungen der Sonne und der inneren Heliosphäre liefert, um dazu beizutragen, den Ursprung, die Entwicklung und die interplanetaren Auswirkungen von koronalen Massenauswürfen zu verstehen.
The main research fields of the department "Sun and Heliosphere" are covered by the research groups "Solar and Stellar Coronae", "Solar Lower Atmosphere and Magnetism", "Solar and Stellar Magnetohydrodynamics" and "Solar Variability and Climate".
The variability of Space Weather originates in the vigorous dynamics above the solar surface. A dominant energy source is the coronal magnetic field. It is set free by instabilities as new field breaks through the surface and its foot points which remain anchored on the surface are continuously convected around. We investigate these processes in detail by modelling the coronal magnetic field and plasma environment from solar surface magnetic measurements and space borne EUV observations.