Chifu, I.; Wiegelmann, T.; Inhester, B.: Coronal magnetic field modeling using stereoscopic constraints. 15th European Solar Physics Meeting, Budapest, Hungary (2017)
Wiegelmann, T.: 3D-Coronal magnetic fields. Theoretical and observational approaches to the solar magnetic field: Achievements and remaining problems - conference in honor of Prof. Takashi Sakurai's career -, Tokyo, Japan (2016)
Wiegelmann, T.: The Magnetic Field of the Sun. AG 2016, Splinter meeting: The Role and Interaction of Stellar Magnetic Fields: From the Stellar Surface to the Interstellar Medium, Bochum, Germany (2016)
Wiegelmann, T.: Coronal modelling for Solar Orbiter. 16th Solar Orbiter SWT Meeting Numerical modeling support for Solar Orbiter (special MADAWG session), Göttingen, Germany (2015)
Wiegelmann, T.: Solar magnetic activity and space weather. Workshop and Research visit on: The synergy of magnetic reconnection and waves in evolution of the solar corona, Weihai, China (2015)
Wiegelmann, T.: Solar coronal magnetic fields: Source region for space weather activity. 4. Nationaler Weltraumwetterworkshop, Neustrelitz, Germany (2015)
Wiegelmann, T.; The Sunrise Team: Selfconsistent magnetostatic modelling of the solar atmosphere from Sunrise/IMAX measurements. AG Annual Meeting 2014, Bamberg, Germany (2014)
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, ...