Tadesse, T.; Wiegelmann, T.; Inhester, B.; Pevtsov, A.: Magnetic Connectivity Between Active Regions 10987, 10988, and 10989 by Means of Nonlinear Force-Free Field Extrapolation. Solar Physics 277, pp. 119 - 130 (2012)
Tadesse, T.; Wiegelmann, T.; Inhester, B.; Pevtsov, A.: Coronal Magnetic Field Structure and Evolution for Flaring AR 11117 and Its Surroundings. Solar Physics 281, pp. 53 - 65 (2012)
Wiegelmann, T.; Thalmann, J. K.; Inhester, B.; Tadesse, T.; Sun, X.; Hoeksema, J. T.: How Should One Optimize Nonlinear Force-Free Coronal Magnetic Field Extrapolations from SDO/HMI Vector Magnetograms? Solar Physics 281, pp. 37 - 51 (2012)
DeRosa, M. L.; Schrijver, C. J.; Barnes, G.; Leka, K. D.; Lites, B. W.; Aschwanden, M. J.; Amari, T.; Canou, A.; McTiernan, J. M.; Régnier, S.et al.; Thalmann, J. K.; Valori, G.; Wheatland, M. S.; Wiegelmann, T.; Cheung, M. C. M.; Conlon, P. A.; Fuhrmann, M.; Inhester, B.; Tadesse, T.: A Critical Assessment of Nonlinear Force-Free Field Modeling of the Solar Corona for Active Region 10953. Astrophysical Journal 696, pp. 1780 - 1791 (2009)
Tadesse, T.; Wiegelmann, T.; Inhester, B.: Nonlinear force-free coronal magnetic field modelling and preprocessing of vector magnetograms in spherical geometry. Astronomy and Astrophysics 508, pp. 421 - 432 (2009)
Tadesse Asfaw, T.: Nonlinear force-free reconstruction of the coronal magnetic field with advanced numerical methods. Dissertation, Georg-August-Universität Göttingen (2011)
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, ...