Weisshaar, E.; Cameron, R. H.; Schüssler, M.: No evidence for synchronization of the solar cycle by a "clock". Astronomy and Astrophysics 671, p. A87 (2023)
Cameron, R. H.; Schüssler, M.: Solar activity: periodicities beyond 11 years are consistent with random forcing. Astronomy and Astrophysics 625, A28 (2019)
Borrero, J. M.; Jafarzadeh, S.; Schüssler, M.; Solanki, S. K.: Solar Magnetoconvection and Small-Scale Dynamo Recent Developments in Observation and Simulation. Space Science Reviews 210 (1-4), pp. 275 - 316 (2017)
Cameron, R.; Schüssler, M.: The turbulent diffusion of toroidal magnetic flux as inferred from properties of the sunspot butterfly diagram. Astronomy and Astrophysics 591, A46 (2016)
Beeck, B.; Schüssler, M.; Cameron, R. H.; Reiners, A.: Three-dimensional simulations of near-surface convection in main-sequence stars - III. The structure of small-scale magnetic flux concentrations. Astronomy and Astrophysics 581, A42 (2015)
Beeck, B.; Schüssler, M.; Cameron, R. H.; Reiners, A.: Three-dimensional simulations of near-surface convection in main-sequence stars - IV. Effect of small-scale magnetic flux concentrations on centre-to-limb variation and spectral lines. Astronomy and Astrophysics 581, A43 (2015)
Hanasoge, S.; Miesch, M. S.; Roth, M.; Schou, J.; Schüssler, M.; Thompson, M. J.: Solar Dynamics, rotation, convection and overshoot. Space Science Reviews 196, pp. 79 - 99 (2015)
Cameron, R. H.; Jiang, J.; Schuessler, M.; Gizon, L.: Physical causes of solar cycle amplitude variability. Journal of Geophysical Research: Space Physics 119, pp. 680 - 688 (2014)
Jiang, J.; Cameron, R. H.; Schüssler, M.: Effects of the scatter in sunspot group tilt angles on the large‐scale magnetic field at the solar surface. Astrophysical Journal 791, 5 (2014)
Reiners, A.; Schüssler, M.; Passegger, V. M.: Generalized investigation of the rotation‐activity relation: Favoring rotation period instead of Rossby number. Astrophysical Journal 794, 144 (2014)
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.