Krivova, N. A.; Solanki, S. K.; Fligge, M.; Unruh, Y. C.: Reconstruction of solar irradiance variations in Cycle 23: Is solar surface magnetism the cause? Astronomy and Astrophysics 399, pp. L1 - L4 (2003)
Knaack, R.; Fligge, M.; Solanki, S. K.; Unruh, Y. C.: The influence of an inclined rotation axis on solar irradiance variations. Astronomy and Astrophysics 376, pp. 1080 - 1089 (2001)
Unruh, Y. C.; Solanki, S. K.; Fligge, M.: Modelling solar irradiance variations: Comparison with observations, including line-ratio variations. Space Science Reviews 94, pp. 145 - 152 (2000)
Knaack, R.; Fligge, M.; Solanki, S. K.; Unruh, Y. C.: Stellar irradiance variations caused by magnetic activity: the influence of an inclined rotation axis. In: Magnetic Fields Across the Hertzsprung-Russell Diagram, pp. 227 - 230 (Eds. Mathys, G.; Solanki, S. K.; Wickramasinghe, D. T.). Astronomical Society of the Pacific, San Francisco/CA (2001)
Solanki, S. K.; Fligge, M.; Unruh, Y. C.: Variations of the solar spectral irradiance. In: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from SOHO and Other Space Missions, pp. 66 - 77 (Eds. Brekke, P.; Fleck, B.; Gurman, J. B.). (2001)
Unruh, Y. C.; Knaack, R.; Fligge, M.; Solanki, S. K.: Are the Sun's brightness variations really tamer than those of other comparable solar-type stars? In: Cool Stars, Stellar Systems and the Sun XI, pp. CD - 748 (Eds. López, G.; J., R.; Rebolo; R.; Osorio, Z. et al.). Astronomical Society of the Pacific, San Francisco (2001)
Fligge, M.; Solanki, S. K.; Meunier, N.; Unruh, Y. C.: Solar surface magnetism and the increase of solar irradiance between activity minimum and maximum. In: Proc. 1st Solar & Space Weather Euroconference ``The Solar Cycle and Terrestrial Climate'', Santa Cruz de Tenerife, Spain, pp. 117 - 121 (Ed. Wilson, A.). ESA Publ. Div., Noordwijk (2000)
Knaack, R.; Fligge, M.; Solanki, S. K.; Unruh, Y. C.: The influence of an inclined rotation axis on solar irradiance variations. In: Proc. Workshop on ``The Sun and Sun-like Stars'', pp. 45 - 52 (Eds. Jankovics, I.; Kovács, J.; Vincze, I. J.). Gothard Astrophysical Observatory, Szombathely, Hungary (2000)
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.