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)
First Light for Sunrise III: the first tests with real sunlight were successful. The balloon-borne solar observatory should be ready for launch at the end of May.
First icy cold, then midnight sun: at the Arctic Circle, the team will prepare the next flight of the balloon-borne solar observatory - and hopes for solar fireworks.
Astronomical teamwork: By combining data from Solar Orbiter and SDO, a group of researchers has unambiguously determined the magnetic field at the solar surface.
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.