Löptien, B.; Lagg, A.; van Noort, M.; Solanki, S. K.: No universal connection between the vertical magnetic field and the umbra-penumbra boundary in sunspots. Astronomy and Astrophysics 639, A106 (2020)
Prabhu, A.; Brandenburg, A.; Käpylä, M. J.; Lagg, A.: Helicity proxies from linear polarisation of solar active regions. Astronomy and Astrophysics 641, A46 (2020)
Prabhu, A.; Lagg, A.; Hirzberger, J.; Solanki, S. K.: The magnetic fine structure of the Sun's polar region as revealed by Sunrise. Astronomy and Astrophysics 644, A86 (2020)
Siu-Tapia, A. L.; Lagg, A.; van Noort, M.; Rempel, M.; Solanki, S. K.: Superstrong photospheric magnetic fields in sunspot penumbrae. Astron. Astrophys.; EDP Sciences, Les Ulis Cedex A France 631, A99 (2019)
González Manrique, S. J.; Kuckein, C.; Collados, M.; Denker, C.; Solanki, S. K.; Gömöry, P.; Verma, M.; Balthasar, H.; Lagg, A.; Diercke, A.: Temporal evolution of arch filaments as seen in He I 10 830 Å. Astronomy and Astrophysics 617, A55 (2018)
Löptien, B.; Lagg, A.; van Noort, M.; Solanki, S. K.: Measuring the Wilson depression of sunspots using the divergence-free condition of the magnetic field vector. Astronomy and Astrophysics 619, A42 (2018)
Singh, N. K.; Käpylä, M. J.; Brandenburg, A.; Käpylä, P. J.; Lagg, A.; Virtanen, I.: Bihelical Spectrum of Solar Magnetic Helicity and Its Evolution. The Astrophysical Journal 863 (2), 182 (2018)
Siu-Tapia, A. L.; Rempel, M.; Lagg, A.; Solanki, S. K.: Evershed and Counter-Evershed Flows in Sunspot MHD Simulations. The Astrophysical Journal 852 (2), 66 (2018)
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, ...