Kretzschmar, M.; Snow, M.; Curdt, W.: An Empirical Model of the Variation of the Solar Lyman-α Spectral Irradiance. Geophysical Research Letters 45 (5), pp. 2138 - 2144 (2018)
Gladstone, G. R.; Stern, S. A.; Ennico, K.; Olkin, C. B.; Weaver, H. A.; Young, L. A.; Summers, M. E.; Strobel, D. F.; Hinson, D. P.; Kammer, J. A.et al.; Parker, A. H.; Steffl, A. J.; Linscott, I. R.; Parker, J. W.; Cheng, A. F.; Slater, D. C.; Versteeg, M. H.; Greathouse, T. K.; Retherford, K. D.; Throop, H.; Cunningham, N. J.; Woods, W. W.; Singer, K. N.; Tsang, C. C. C.; Schindhelm, E.; Lisse, C. M.; Wong, M. L.; Yung, Y. L.; Zhu, X.; Curdt, W.; Lavvas, P.; Young, E. F.; Tyler, G. L.; the New Horizons Science Team: The atmosphere of Pluto as observed by New Horizons. Science 351, aaf8866 (2016)
Avrett, E.; Tian, H.; Landi, E.; Curdt, W.; Wülser, J.-P.: Modeling the chromosphere of a sunspot and the quiet sun. Astrophysical Journal 811, pp. 87 - 103 (2015)
Giunta, A. S.; Fludra, A.; Lanzafame, A. C.; O'Mullane, M. G.; Summers, H. P.; Curdt, W.: On extreme-ultraviolet helium line intensity enhancement factors on the Sun. Astrophysical Journal 803, 66 (2015)
Lemaire, P.; Vial, J.-C.; Curdt, W.; Schühle, U.; Wilhelm, K.: Hydrogen Ly-α and Ly-β full Sun line profiles observed with SUMER/SOHO (1996-2009). Astronomy and Astrophysics 581, A26, pp. 1 - 7 (2015)
Vial, J.-C.; Eurin, G.; Curdt, W.: The Balmer lines of He II in the blue wing of the hydrogen Lyman alpha line observed in a quiescent prominence. Solar Physics 290, pp. 381 - 387 (2015)
Wang, X.; McIntosh, S. W.; Curdt, W.; Tian, H.; Peter, H.; Xia, L.-D.: Temperature dependence of ultraviolet line parameters in network and internetwork regions of the quiet Sun and coronal holes. Astronomy and Astrophysics 557, A126 (2013)
Analyzing the high spatial resolution solar Ca II H and K emission data obtained by the SUNRISE mission and building a model of other stars more active than the Sun
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.
For PhD students whose project is already funded and who are applying for admission to the IMPRS, or for applicants who want to bring their own funding and their own project idea to the IMPRS.
The Solar Lower Atmosphere and Magnetism (SLAM) group covers many exciting subjects in solar physics, focussing on the development and testing of highly novel solar instrumentation, reduction and analysis of highest quality solar observations, or improving and developing advanced techniques for the analysis of solar observations.