Beeck, B.; Cameron, R. H.; Reiners, A.; Schüssler, M.: Three-dimensional simulations of near-surface convection in main-sequence stars II. Properties of granulation and spectral lines. Astronomy and Astrophysics 558, A49 (2013)
Beeck, B.; Collet, R.; Steffen, M.; Asplund, M.; Cameron, R. H.; Freytag, B.; Hayek, W.; Ludwig, H.-G.; Schüssler, M.: Simulations of the solar near-surface layers with the CO5BOLD, MURaM, and Stagger codes. Astronomy and Astrophysics 539, A121 (2012)
Cameron, R. H.; Schüssler, M.: Are the strengths of solar cycles determined by converging flows towards the activity belts? Astronomy and Astrophysics 548, A57 (2012)
Moll, R.; Cameron, R. H.; Schüssler, M.: Vortices, shocks, and heating in the solar photosphere: effect of a magnetic field. Astronomy and Astrophysics 541, A68 (2012)
Afram, N.; Unruh, Y. C.; Solanki, S. K.; Schüssler, M.; Lagg, A.; Vögler, A.: Intensity contrast from MHD simulations and HINODE observations. Astronomy and Astrophysics 526, A120 (2011)
Cameron, R. H.; Vögler, A...; Schüssler, M.: Decay of a simulated mixed-polarity magnetic field in the solar surface layers. Astronomy and Astrophysics 533, A86 (2011)
Jiang, J.; Cameron, R. H.; Schmitt, D.; Schüssler, M.: The solar magnetic field since 1700 I. Characteristics of sunspot group emergence and reconstruction of the butterfly diagram. Astronomy and Astrophysics 528, A82 (2011)
Jiang, J.; Cameron, R. H.; Schmitt, D.; Schüssler, M.: The solar magnetic field since 1700 II. Physical reconstruction of total, polar and open flux. Astronomy and Astrophysics 528, A83 (2011)
Röhrbein, D.; Cameron, R.; Schüssler, M.: Is there a non-monotonic relation between photospheric brightness and magnetic field strength? Astronomy and Astrophysics 532, A140 (2011)
The research group “Solar Lower Atmosphere and Magnetism” (SLAM) studies the conditions and dynamic processes in the atmospheric layer between the solar surface (photosphere) and the overlying chromosphere, an approximately 2000 km thick gas layer.
The main research fields of the department "Sun and Heliosphere" are covered by the research groups "Solar and Stellar Coronae", "Solar Lower Atmosphere and Magnetism", "Solar and Stellar Magnetohydrodynamics" and "Solar Variability and Climate".
How does our star heat its outer atmosphere, the solar corona, to unimaginable temperatures of up to 10 million degrees Celsius? With unprecedented observational data from ESA's Solar Orbiter spacecraft and powerful computer simulations, ERC starting grant awardee Pradeep Chitta intends to bring new momentum to the search for the coronal heating mechanism.