Curdt, W.; Tian, H.; Dwivedi, B. N.; Marsch, E.: The redshifted network contrast of transition region emission. Astronomy and Astrophysics 491, pp. L13 - L16 (2008)
Curdt, W.; Tian, H.; Teriaca, L.; Schühle, U.; Lemaire, P.: The Ly-α profile and center-to-limb variation of the quiet Sun. Astronomy and Astrophysics 492, pp. L9 - L12 (2008)
Marsch, E.; Tian, H.; Sun, J.; Curdt, W.; Wiegelmann, T.: Plasma flows guided by strong magnetic fields in the solar corona. Astrophysical Journal 685, pp. 1262 - 1269 (2008)
Teriaca, L.; Curdt, W.; Solanki, S. K.: SUMER observations of the inverse Evershed effect in the transition region above a sunspot. Astronomy and Astrophysics 491, pp. L5 - L8 (2008)
Wilhelm, K.; Curdt, W.; Dammasch, I. E.; Hassler, D. M.: Comment on ``Energy levels and spectral lines of NeVIII''. Eur. Phys. J. D 47 (3), p. 325 - 325 (2008)
Fontenla, J. M.; Curdt, W.; Avrett, E. H.; Harder, J.: Log-normal intensity distribution of the quiet-Sun FUV continuum observed by SUMER. Astronomy and Astrophysics 468, pp. 695 - 699 (2007)
Madjarska, M. S.; Doyle, J. G.; Innes, D. E.; Curdt, W.: Jets or High-Velocity Flows Revealed in High-Cadence Spectrometer and Imager Co-observations? Astrophysical Journal 670, pp. L57 - L60 (2007)
McIntosh, S. W.; Davey, A. R.; Hassler, D. M.; Armstrong, J. D.; Curdt, W.; Wilhelm, K.; Lin, G.: Observations supporting the role of magnetoconvection in energy supply to the quiescent solar atmosphere. Astrophysical Journal 654, pp. 650 - 664 (2007)
Emerich, C.; Lemaire, P.; Vial, J.-C.; Curdt, W.; Schühle, U.; Wilhelm, K.: A new relation between the central spectral solar H I Lyman α irradiance and the line irradiance measured by SUMER/SOHO during the cycle 23. Icarus 178, pp. 429 - 433 (2005)
Gömöry, P.; Rybak, J.; Kucera, A.; Curdt, W.; Wöhl, H.: Variability and dynamics of the outer atmospheric layers in the quiet solar network. Hvar Obs. Bull. 29, pp. 71 - 78 (2005)
Lemaire, P.; Emerich, C.; Vial, J.-C.; Curdt, W.; Schühle, U.; Wilhelm, K.: Variation of the full Sun hydrogen Lyman profiles through solar cycle 23. Advances in Space Research 35, pp. 384 - 387 (2005)
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.