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Showing 1 to 4 of 4 for “"Mars Express"”.

  1. Dynamique et composition des atmosphères supérieures de Mars et Vénus observées par les spectrographes ultraviolets à bord de Mars Express et Vénus Express

    … by the SPICAV instrument on board the ESA Venus Express spacecraft. I discuss the altitude and brightness of the emission peak (60 kR at 115 km) and show that the emission profile exhibits a secondary peak in ~10% of the cases. This additional peak is probably caused by upward-moving gravity …

    liege Repository record for Dynamique et composition des atmosphères supérieures de Mars et Vénus observées par les spectrographes ultraviolets à bord de Mars Express et Vénus Express (opens in a new tab)

  2. Infrared Spectra Analysis of Thermally Altered Iron Phyllosilicates and the Implications for Mars

    … phyllosilicates, which may be present on Mars. The minerals, greenalite and hisingerite, are rich in iron-II and iron-III, respectively. Small samples (~0.40 grams) of each mineral were crushed and heated in a Lindberg Tube Oven for approximately twenty-four hours at temperatures selected …

    arkansas Repository record for Infrared Spectra Analysis of Thermally Altered Iron Phyllosilicates and the Implications for Mars (opens in a new tab)

  3. Entwicklung, Implementierung und Erprobung eines planetaren Informationssystems auf Basis von ArcGIS

    … der Berechnung der Oberflächenrauigkeit der Marsoberfläche inklusive der flächendeckenden Kalibrierung der Eingangs-Basisdaten. Exemplarisch konnte gezeigt werden, dass das Verfahren eine verbesserte Berechnung der Oberflächenrauigkeit ermöglicht, als bisher angewandte Ansätze. Zudem wurde …

    potsdam-diss Repository record for Entwicklung, Implementierung und Erprobung eines planetaren Informationssystems auf Basis von ArcGIS (opens in a new tab)

  4. Remote Sensing and Terramechanics Study of Mars using Orbital and Rover Data Sets

    … weakly altered basaltic sands. Comparison of Mars Odyssey THEMIS-derived thermal inertia values with Mars Express OMEGA-derived spectral parameters shows that although the dust cover can be optically thick: 0.4 to 2.5 μm wavelength region) in some areas, it is not thick enough: ~1 cm) to …

    wustl Repository record for Remote Sensing and Terramechanics Study of Mars using Orbital and Rover Data Sets (opens in a new tab)