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Kallinger, T.; Hekker, S.; Garcia, R. A.; Huber, D.; Matthews, J. M.: Precise stellar surface gravities from the time scales of convectively driven brightness variations. Science Advances 2, e1500654 (2016)
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van Lieshout, R.; Min, M.; Dominik, C.; Brogi, M.; de Graaff, T.; Hekker, S.; Kama, M.; Keller, C. U.; Ridden-Harper, A.; van Werkhoven, T. I. M.: Dusty tails of evaporating exoplanets. II. Physical modelling of the KIC 12557548b light curve. Astronomy and Astrophysics 596, A32 (2016)
Alam, S.; Albareti, F. D.; Allende Prieto, C.; Anders, F.; Anderson, S. F.; Anderton, T.; Andrews, B. H.; Armengaud, E.; Aubourg, É.; Bailey, S.et al.; Hekker, S.; et al.: The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data from SDSS-III. Astrophysical Journal, Suppl. Ser. 219, 12 (2015)
Campante, T. L.; Barclay, T.; Swift, J. J.; Huber, D.; Adibekyan, V. Z.; Cochran, W.; Burke, C. J.; Isaacson, H.; Quintana, E. V.; Davies, G. R.et al.; Silva Aguirre, V.; Ragozzine, D.; Riddle, R.; Baranec, C.; Basu, S.; Chaplin, W. J.; Christensen-Dalsgaard, J.; Metcalfe, T. S.; Bedding, T. R.; Handberg, R.; Stello, D.; Brewer, J. M.; Hekker, S.; Karoff, C.; Kolbl, R.; Law, N. M.; Lundkvist, M.; Miglio, A.; Rowe, J. F.; Santos, N. C.; Van Laerhoven, C.; Arentoft, T.; Elsworth, Y. P.; Fischer, D. A.; Kawaler, S. D.; Kjeldsen, H.; Lund, M. N.; Marcy, G. W.; Sousa, S. G.; Sozzetti, A.; White, T. R.: An Ancient Extrasolar System with Five Sub-Earth-size Planets. Astrophysical Journal 799, 170 (2015)
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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, ...