Bekki, Y.; Cameron, R. H.; Gizon, L.: Theory of solar oscillations in the inertial frequency range: Amplitudes of equatorial modes from a nonlinear rotating convection simulation. Astronomy and Astrophysics 666, p. A135 (2022)
Bekki, Y.; Cameron, R. H.; Gizon, L.: Theory of solar oscillations in the inertial frequency range: Linear modes of the convection zone. Astronomy and Astrophysics 662, p. A16 (2022)
Bhatia, T. S.; Cameron, R. H.; Solanki, S. K.; Peter, H.; Przybylski, D.; Witzke, V.; Shapiro, A.: Small-scale dynamo in cool stars. I. Changes in stratification and near-surface convection for main-sequence spectral types. Astronomy and Astrophysics 663, p. A166 (2022)
Biswas, A.; Karak, B. B.; Cameron, R.: Toroidal Flux Loss due to Flux Emergence Explains why Solar Cycles Rise Differently but Decay in a Similar Way. Physical Review Letters 129, p. 241102 (2022)
Gottschling, N.; Schunker, H.; Birch, A.; Cameron, R. H.; Gizon, L.: Testing solar surface flux transport models in the first days after active region emergence. Astronomy and Astrophysics 660, A6 (2022)
Gottschling, N.; Schunker, H.; Birch, A. C.; Cameron, R.; Gizon, L.: Testing solar surface flux transport models in the first days after active region emergence. Astronomy and Astrophysics 660, p. A6 (2022)
Jeffers, S. V.; Cameron, R. H.; Marsden, S. C.; Boro Saikia, S.; Folsom, C. P.; Jardine, M. M.; Morin, J.; Petit, P.; See, V.; Vidotto, A. A.et al.; Wolter, U.; Mittag, M.: The crucial role of surface magnetic fields for stellar dynamos: ϵ Eridani, 61 Cygni A, and the Sun. Astronomy and Astrophysics 661, p. A152 (2022)
Witzke, V.; Shapiro, A. I.; Kostogryz, N. M.; Cameron, R.; Rackham, B. V.; Seager, S.; Solanki, S. K.; Unruh, Y. C.: Can 1D Radiative-equilibrium Models of Faculae Be Used for Calculating Contamination of Transmission Spectra? The Astrophysical Journal 941, p. L35 (2022)
Harra, L.; Andretta, V.; Appourchaux, T.; Baudin, F.; Bellot-Rubio, L.; Birch, A.; Boumier, P.; Cameron, R. H.; Carlsson, M.; Corbard, T.et al.; Davies, J.; Fazakerley, A.; Fineschi, S.; Finsterle, W.; Gizon, L.; Harrison, R.; Hassler, D.M.; Leibacher, J.; Liewer, P.; Macdonald, M.; Maksimovic, M.; Murphy, N.; Naletto, G.; Nigro, G.; Owen, C.; Martínez-Pillet, V.; Rochus, P.; Romoli, M.; Sekii, T.; Spadaro, D.; Veronig, A.; Schmutz, W.: A journey of exploration to the polar regions of a star: probing the solar poles and the heliosphere from high helio-latitude. Experimental Astronomy (2021)
Panja, M.; Cameron, R. H.; Solanki, S. K.: Sunspot Simulations: Penumbra Formation and the Fluting Instability. The Astrophysical Journal 907 (2), 102 (2021)
Yadav, N.; Cameron, R. H.; Solanki, S. K.: Vortex flow properties in simulations of solar plage region: Evidence for their role in chromospheric heating. Astronomy and Astrophysics 645, A3 (2021)
Yadav, N.; Cameron, R. H.; Solanki, S. K.: Slow magneto-acoustic waves in simulations of a solar plage region carry enough energy to heat the chromosphere. Astronomy and Astrophysics 652, A43 (2021)
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.