Schröder, S. E.; Keller, H. U.: The unusual phase curve of Titan's surface observed by Huygens Descent Imager/Spectral Radiometer. Planetary and Space Science 57, pp. 1963 - 1974 (2009)
Sizemore, H. G.; Mellon, M. T.; Searls, M. L.; Lemmon, M. T.; Zent, A. P.; Heet, T. L.; Arvidson, R. E.; Blaney, D. L.; Keller, H. U.: Rocks of the Phoenix Landing Site. Journal Geophysical Research 115, E00E09 (2009)
Smith, P. H.; Tamppari, L. K.; Arvidson, R. E.; Bass, D.; Blaney, D.; Boynton, W. V.; Carswell, A.; Catling, D. C.; Clark, B. C.; Duck, T.et al.; DeJong, E.; Fisher, D.; Goetz, W.; Gunnlaugsson, H. P.; Hecht, M. H.; Hipkin, V.; Hoffman, J.; Hviid, S. F.; Keller, H. U.; Kounaves, S. P.; Lange, C. F.; Lemmon, M. T.; Madsen, M. B.; Markiewicz, W. J.; Marshall, J.; Mckay, C. P.; Mellon, M. T.; Ming, D. W.; Morris, R. V.; Pike, W. T.; Renno, N.; Staufer, U.; Stoker, C.; Taylor, P.; Whiteway, J. A.; Zent, A. P.: H2O at the Phoenix Landing Site. Science 325 (5936), pp. 58 - 61 (2009)
Hecht, M. H.; Marshall, J.; Pike, W. T.; Staufer, U.; Blaney, D.; Braendlin, D.; Gautsch, S.; Goetz, W.; Hidber, H.-R.; Keller, H. U.et al.; Markiewicz, W. J.; Mazer, A.; Meloy, T. P.; Morookian, J. M.; Mogensen, C.; Parrat, D.; Smith, P.; Sykulska, H.; Tanner, R. J.; Reynolds, R. O.; Tonin, A.; Vijendran, S.; Weilert, M.; Woida, P. M.: Microscopy capabilities of the Microscopy, Electrochemistry, and Conductivity Analyzer. Journal Geophysical Research 113, E00A22 (2008)
Inada, A.; Garcia-Comas, M.; Altieri, F.; Gwinner, K.; Poulet, F.; Bellucci, G.; Keller, H. U.; Markiewicz, W. J.; Richardson, M. I.; Hoekzema, N.et al.; Neukum, G.; Bibring, J.-P.: Dust haze in Valles Marineris observed by HRSC and OMEGA on board Mars Express. Journal Geophysical Research 113, E02004 (2008)
Maltagliati, L.; Titov, D. V.; Encrenaz, T.; Melchiorri, R.; Forget, F.; Garcia-Comas, M.; Keller, H. U.; Langevin, Y.; Bibring, J.-P.: Observations of atmospheric water vapor above the Tharsis volcanoes on Mars with the OMEGA/MEx imaging spectrometer. Icarus 194 (1), pp. 53 - 64 (2008)
Schröder, S. E.; Keller, H.-U.: The reflectance spectrum of Titan's surface at the Huygens landing site determined by the Descent Imager/Spectral Radiometer. Planetary and Space Science 56, pp. 753 - 769 (2008)
Skorov, Y. V.; Keller, H. U.; Rodin, A. V.: Optical properties of aerosols in Titan's atmosphere. Planetary and Space Science 56 (5), pp. 660 - 668 (2008)
Basilevsky, A. T.; Keller, H. U.: Craters, smooth terrains, flows, and layering on the comet nuclei. Solar System Research 41 (2), pp. 109 - 117 (2007)
Jorda, L.; Lamy, P.; Faury, G.; Keller, H. U.; Hviid, S.; Küppers, M.; Koschny, D.; Lecacheux, J.; Gutiérrez, P.; Lara, L. M.: Properties of the dust cloud caused by the Deep Impact experiment. Icarus 187, pp. 208 - 219 (2007)
Küppers, M.; Keller, H. U.; Kührt, E.; the CNSR Team: A comet nucleus sample return (CNSR) mission in ESAs Cosmic Vision program. Geochim. Cosmochim. Acta 71, p. A531 (2007)
Küppers, M.; Mottola, S.; Lowry, S. C.; A'Hearn, M. A.; Barbieri, C.; Barucci, M. A.; Fornasier, S.; Groussin, O.; Gutiérrez, P.; Hviid, S. F.et al.; Keller, H. U.; Lamy, P.: Determination of the light curve of the Rosetta target asteroid (2867) Steins by the OSIRIS cameras onboard Rosetta. Astronomy and Astrophysics 462, pp. L13 - L16 (2007)
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
The Planetary Plasma Environments group (PPE) has a strong heritage in the exploration of planetary magnetospheres and space plasma interactions throughout the solar system. It has contributed instruments to several past missions that flew-by or orbited Jupiter (Galileo, Cassini, Ulysses). The PPE participates in the JUICE mission by contributing hardware and scientific expertise to the Particle Environment Package (PEP).
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.