Hamilton, D. C.; Brown, D. C.; Gloeckler, G.; Axford, W. I.: Energetic atomic and molecular ions in Saturn's magnetosphere. Journal Geophysical Research 88, pp. 8905 - 8922 (1983)
McKenzie, J. F.; Axford, W. I.: Comment on 'On rotational forces in the solar wind' by J. V. Hollweg and P. A. Isenberg. Journal Geophysical Research 88, pp. 7251 - 7252 (1983)
Webb, G.; Axford, W. I.; Terasawa, T.: On the drift mechanism for energetic charged particles at shocks. Astrophysical Journal 270, pp. 537 - 553 (1983)
Krimigis, S. M.; Armstrong, T. P.; Axford, W. I.; Bostrom, C. O.; Gloeckler, G.; Keath, E. P.; Lanzerotti, L. J.; Carbary, J. F.; Hamilton, D. C.; Roelof, E. C.: Low energy hot plasma and particles in Saturn's magnetosphere. Science 215, pp. 571 - 577 (1982)
Carbary, J. F.; Krimigis, S. M.; Keath, E. P.; Gloeckler, G.; Axford, W. I.; Armstrong, T. P.: Ion anisotropies in the outer Jovian magnetosphere. Journal Geophysical Research 86, pp. 8285 - 8299 (1981)
Krimigis, S. M.; Armstrong, T. P.; Axford, W. I.; Bostrom, C. O.; Gloeckler, G.; Keath, E. P.; Lanzerotti, L. J.; Carbary, J. F.; Hamilton, D. C.; Roelof, E. C.: Low-energy charged particles in Saturn's magnetosphere: Results form Voyager 1. Science 212, pp. 225 - 231 (1981)
Krimigis, S. M.; Carbary, J. F.; Keath, E. P.; Bostrom, C. O.; Axford, W. I.; Gloeckler, G.; Lanzerotti, L. J.; Armstrong, T. P.: Characteristics of hot plasma in the Jovian magnetosphere: Results from the Voyager spacecraft. Journal Geophysical Research 86, pp. 8227 - 8257 (1981)
Hamilton, D. C.; Gloeckler, G.; Krimigis, S. M.; Bostrom, C. O.; Armstrong, T. P.; Axford, W. I.; Fan, C. Y.; Lanzerotti, L. J.; Hunten, D. M.: Detection of energetic hydrogen molecules in Jupiter's magnetosphere by Voyager 2: Evidence for an ionospheric plasma source. Geophysical Research Letters 7, pp. 813 - 816 (1980)
Krimigis, S. M.; Armstrong, T. P.; Axford, W. I.; Bostrom, C. O.; Fan, C. Y.; Gloeckler, G.; Lanzerotti, L. J.; Hamilton, D. C.; Zwickl, R. D.: Energetic (∼ 100 keV) tailward-directed ion beam outside the Jovian plasma boundary. Geophysical Research Letters 7, pp. 13 - 16 (1980)
Krimigis, S. M.; Armstrong, T. P.; Axford, W. I.; Bostrom, C. O.; Fan, C. Y.; Gloeckler, G.; Lanzerotti, L. J.; Keath, E. P.; Zwickl, R. D.; Carbary, J. F.et al.; Hamilton, D. C.: Low-energy charged particle environment at Jupiter: A first look. Science 204, pp. 998 - 1003 (1979)
Krimigis, S. M.; Armstrong, T. P.; Axford, W. I.; Bostrom, C. O.; Fan, C. Y.; Gloeckler, G.; Lanzerotti, L. J.; Keath, E. P.; Zwickl, R. D.; Carbary, J. F.et al.; Hamilton, D. C.: Hot plasma environment at Jupiter: Voyager 2 results. Science 206, pp. 977 - 984 (1979)
Lanzerotti, L. J.; Krimigis, S. M.; Bostrom, C. O.; Axford, W. I.; Lepping, R. P.; Ness, N. F.: Measurements of plasma flow at the dawn magnetopause by Voyager 1. Journal Geophysical Research 84, pp. 6483 - 6488 (1979)
McKenzie, J. F.; Ip, W.-H.; Axford, W. I.: The acceleration of minor ion species in the solar wind. Astrophys. and Space Phys. 64, pp. 183 - 211 (1979)
Richter, A. K.; Keppler, E.; Axford, W. I.; Denskat, K. U.: Dynamics of low-energy electrons (gt; 17 keV) and ions (gt; 80 keV) in the vicinity of the low-latitude, duskside magnetopause: Helios 1 and 2 observations. Journal Geophysical Research 84, pp. 1453 - 1463 (1979)
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.
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.