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Hefti, S.; Grünwaldt, H.; Bochsler, P.; Aellig, M. R.: Oxygen freeze-in temperatures measured with SOHO/CELIAS/CTOF. Journal Geophysical Research 105, p. 10527 (2000)
Aellig, M. R.; Bochsler, P.; Grünwaldt, H.; Hefti, S.; Wurz, P.; Hilchenbach, M.; Hovestadt, D.; Ipavich, F. M.; Gliem, F.: The Influence of Suprathermal Electrons on the Derivation of Coronal Electron Temperatures from Solar Wind Motor Ion Charge States. Physics and Chemistry of the Earth C24, pp. 407 - 414 (1999)
Aellig, M. R.; Hefti, S.; Grünwaldt, H.; Bochsler, P.; Wurz, P.; Ipavich, F. M.; Hovestadt, D.: The Fe/O elemental abundance ratio in the solar wind as observed with SOHO CELIAS CTOF. Journal Geophysical Research 104 (A11), pp. 24769 - 24780 (1999)
Kallenbach, R.; Ipavich, F. M.; Kucharek, H.; Bochsler, P.; Galvin, A. B.; Geiss, J.; Gliem, F.; Gloeckler, G.; Grünwaldt, H.; Hilchenbach, M.et al.; Hovestadt, D.: Solar wind isotopic abundance ratios of Ne, Mg, and Si measured by SOHO/CELIAS/MTOF as diagnostic tool for the inner corona. Physics and Chemistry of the Earth 24C (4), pp. 415 - 419 (1999)
Möbius, E.; Litvinenko, Y.; Grünwaldt, H.; Aellig, M. R.; Bogdanov, A.; Ipavich, F. M.; Bochsler, P.; Hilchenbach, M.; Judge, D.; Klecker, B.et al.; Lee, M. A.; Ogawa, H.: Direct evidence of the interstellar gas flow velocity in the pickup ion cut-off as observed with SOHO CELIAS CTOF. Geophysical Research Letters 26 (20), pp. 3181 - 3184 (1999)
Wurz, P.; Aellig, M. R.; Ipavich, F. M.; Hefti, S.; Bochsler, P.; Galvin, A. B.; Grünwaldt, H.; Hilchenbach, M.; Gliem, F.; Hovestadt, D.: The iron, silicon, and oxygen abundance in the solar wind measured with SOHO/CELIAS/MTOF. Physics and Chemistry of the Earth 24C (4), pp. 421 - 426 (1999)
Aellig, M. R.; Grünwaldt, H.; Bochsler, P.; Wurz, P.; Hefti, S.; Kallenbach, R.; Ipavich, F. M.; Axford, W. I.; Balsiger, H.; Bürgi, A.et al.; Coplan, M. A.; Galvin, A. B.; Geiss, J.; Gliem, F.; Gloeckler, G.; Hilchenbach, M.; Hovestadt, D.; Hsieh, K. C.; Klecker, B.; Lee, M. A.; Livi, S.; Managadze, G. G.; Marsch, E.; Möbius, E.; Neugebauer, M.; Reiche, K.-U.; Scholer, M.; Verigin, M. I.; Wilken, B.: Iron freeze-in temperatures measured by SOHO/CELIAS/CTOF. Journal Geophysical Research 103, pp. 17215 - 17222 (1998)
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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.
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.