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)
First Light! The spectro-polarimeter of the world's largest solar telescope in Hawaii looks at the Sun for the first time. The instrument was developed in Germany.
Dr. Theodosios Chatzistergos receives award by the European Space Weather and Space Climate Association for his research findings on the historical activity of the Sun.
The Zdenĕk Švetska Senior Prize of the Solar Physics Division of the European Physical Society (EPS) recognizes Solanki’s pioneering contributions to solar research.
The magnetic field in the solar atmosphere exceeds the geomagnetic field strength by four orders of magnitude. It greatly influences the processes of energy transport within the solar atmosphere, and dominates the morphology of the solar chromosphere and corona. Kinetic energy from convective motions in the Sun can be efficiently stored in magnetic fields and subsequently released - to heat the solar corona to several million degrees or to blast off coronal mass ejections.
Application deadline 1 October 2024. PhD projects in planetary science, solar and stellar physics, solar magnetism, heliophysics, helioseismology, asteroseismology, ...