Wilhelm, K.; Dwivedi, B. N.: An explanation of the Pioneer anomaly involving accelerated atomic clocks. Astrophysics and Space Sciences Transactions 7, pp. 487 - 494 (2011)
Gabriel, A.; Bely-Dubau, F.; Tison, E.; Wilhelm, K.: The Structure and Origin of Solar Plumes: Network Plumes. Astrophysical Journal 700, pp. 551 - 558 (2009)
Mendoza-Torres, J. E.; Wilhelm, K.; Lara, A.: The solar plasma conditions in the source regions of two explosive events. Astronomy and Astrophysics 495 (2), pp. 613 - 620 (2009)
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)
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)
Wilhelm, K.; Marsch, E.; Dwivedi, B. N.; Feldman, U.: Observations of the Sun at Vacuum-Ultraviolet Wavelengths from Space. Part II: Results and Interpretations. Space Science Reviews 133, pp. 103 - 179 (2007)
Wilhelm, K.: Solar VUV measurements obtained by SOHO instruments and their radiometric calibration. Advances in Space Research 37 (2), pp. 225 - 233 (2006)
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)
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)
Mendoza-Torres, J. E.; Torres-Papqui, J. P.; Wilhelm, K.: Explosive events in the solar atmosphere seen in extreme-ultraviolet emission lines. Astronomy and Astrophysics 431, pp. 339 - 344 (2005)
Wilhelm, K.; Fludra, A.; Teriaca, L.; Harrison, R. A.; Dwivedi, B. N.; Pike, C. D.: The widths of vacuum-ultraviolet spectral lines in the equatorial solar corona observed with CDS and SUMER. Astronomy and Astrophysics 435, pp. 733 - 741 (2005)
Wilhelm, K.; Schühle, U.; Curdt, W.; Hilchenbach, M.; Marsch, E.; Lemaire, P.; Bertaux, J.-L.; Jordan, S. D.; Feldman, U.: On the nature of the unidentified solar emission near 117 nm. Astronomy and Astrophysics 439, pp. 701 - 711 (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
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 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.
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.