Teriaca, L.; Wiegelmann, T.; Lagg, A.; Solanki, S. K.; Curdt, W.; Sekii, T.; the Team, H.: Loop morphology and flows and their relation to the magnetic field. In: First Results from Hinode, p. 196 (Eds. Matthews, S.; Davis, J. M.; Harra, L. K.). (2008)
Madjarska, M. S.; Wiegelmann, T.: Evolution of coronal hole boundaries seen in EIT 195 Å and TRACE 171 Å images. In: Modern Solar Facilities - Advanced Solar Science, pp. 249 - 252 (Eds. Kneer, F.; Puschmann, K. G.; Wittmann, A. D.). Universitätverlag Göttingen (2007)
Wiegelmann, T.; Solanki, S. K.; Lagg, A.; Yelles, L.: Nonlinear force-free magnetic field modelling for VIM on SO. In: The Second Solar Orbiter Workshop (Eds. Marsch, E.; Tsinganos, K.; Marsden, R.; Conroy, L.). ESA Publ. Div., Noordwijk (2007)
Wiegelmann, T.: Non-Linear Force-Free Magnetic Fields. In: Proceedings of the International Scientific Conference on Chromospheric and Coronal Magnetic Fields (Eds. Innes, D. E.; Lagg, A.; Solanki, S. K.; Danesy, D.). ESA Publ. Div., Noordwijk (2005)
Wiegelmann, T.; Lagg, A.; Solanki, S. K.; Inhester, B.; Woch, J.: Magnetic loops: A comparison of extrapolations from the photosphere with chromospheric measurements. In: Proceedings of the International Scientific Conference on Chromospheric and Coronal Magnetic Fields (Eds. Innes, D. E.; Lagg, A.; Solanki, S. K.; Danesy, D.). ESA Publ. Div., Noordwijk (2005)
Wiegelmann, T.; Solanki, S. K.: Why are coronal holes indistinguishable from the quiet sun in transition region radiation? In: Proc. SOHO 15 `Coronal Heating', pp. 35 - 40 (Eds. Walsh, R. W.; Ireland, J.; Danesy, D.; Fleck, B.). ESA Publ. Div., Noordwijk (2004)
Büchner, J.; Nikutowski, B.; Vasyliūnas, V.; Woch, J.; Wiegelmann, T.; Axford, I.; Baumjohann, W.; Glassmeier, K.-H.; Auster, H.-U.; Fornacon, K.-H.et al.; Zelenyi, L. M.; Galperin, Y. I.; Savin, S. P.; Veselov, M. V.; Klimov, S. I.: SCHWARM - a swarm of small spacecraft to study plasma turbulence and magnetic field annihilation. In: Proc. 14th ESA Symposium on European Rocket and Balloon Programmes and Related Research, Potsdam, Germany, 31st May - 3rd June 1999, pp. 615 - 620 (Ed. Kaldeich-Schürmann, B.). ESA Publ. Div., Noordwijk (1999)
Wiegelmann, T.; Chifu, I.; Inhester, B.: Global coronal magnetic field modelling for Solar Orbiter. SPICE Operations Consortium Meeting , Göttingen, Germany (2019)
Wiegelmann, T.: Results of global NLFFF modeling for ISSI-meeting on Linking the Sun to the heliosphere using composition data and modelling. ISSI-meeting on „Linking the Sun to the heliosphere using composition data and modelling", Berne, Switzerland (2019)
Wiegelmann, T.; Neukirch, T.; Nickeler, D. H.; Chifu, I.; Inhester, B.: Global coronal magnetic field modelling: new models. ISSI-meeting on „Linking the Sun to the heliosphere using composition data and modelling", Berne, Switzerland (2019)
Wiegelmann, T.: Global non-potential coronal magnetic field models. Third working meeting on Use of Vector Synoptic Maps for Modeling, Göttingen, Germany (2018)
Wiegelmann, T.; Chifu, I.; Inhester, B.: Global magnetic field modelling for the Solar Orbiter mission. 6th Metis Workshop with Focus on Operations, Göttingen, Germany (2018)
Wiegelmann, T.; Chifu, I.; Inhester, B.: Global magnetic field modelling for the Solar Orbiter mission. Mini-Workshop on Solar Magnetic Field at the Purple Mountain Observatory, Nanjing, Nanjing, China (2018)
Chifu, I.; Wiegelmann, T.; Inhester, B.: Nonlinear force-free coronal magnetic stereoscopy. SOLARNET IV, The Physics of the Sun from the Interior to the Outer Atmosphere, Lanzarote, Spain (2017)
How does our star heat its outer atmosphere, the solar corona, to unimaginable temperatures of up to 10 million degrees Celsius? With unprecedented observational data from ESA's Solar Orbiter spacecraft and powerful computer simulations, ERC starting grant awardee Pradeep Chitta intends to bring new momentum to the search for the coronal heating mechanism.
The research group “Solar Lower Atmosphere and Magnetism” (SLAM) studies the conditions and dynamic processes in the atmospheric layer between the solar surface (photosphere) and the overlying chromosphere, an approximately 2000 km thick gas layer.
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".