HR: 1340h
AN: P33A-0227    [Abstracts]
TI: Observing the surface of Venus with VIRTIS
AU: * Marinangeli, L
EM: luciam@irsps.unich.it
AF: IRSPS - Universita' d'Annunzio, Viale Pindaro 42, Pescara, 65127 Italy
AU: Helbert, J
EM: joern.helbert@dlr.de
AF: DLR - Institute of Planetary Research, Rutherfordstrasse 2, Berlin, 12489 Germany
AU: Kostama, P
EM: petri.kostama@oulu.fi
AF: University of Oulu, Linnanmaa, Oulu, 90014 Finland
AU: Baines, K
EM: kbaines@mail1.jpl.nasa.gov
AF: Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, 91109 United States
AU: Garcia, R
EM: garcia@ipgp.jussieu.fr
AF: Institut de Physique du Globe de Paris, 4 ave de Neptune, Paris, 94107 France
AU: Langevin, Y
EM: yves.langevin@ias.u-psud.fr
AF: Institut d'Astrophysique Spatiale, Bƒtiment 121, Orsay, 91405 France
AU: Benkhoff , J
EM: johannes.benkhoff@dlr.de
AF: DLR - Institute of Planetary Research, Rutherfordstrasse 2, Berlin, 12489 Germany
AU: Drossart, P
EM: pierre.drossart@obspm.fr
AF: LESIA - Observatoire de Paris, 61 avenue de l'observatoire, Paris, 75014 France
AU: Piccioni, G
EM: piccioni@rm.iasf.cnr.it
AF: INAF, Via del Fosso del Cavaliere 100, Roma, 00133 Italy
AB: Venus Express Mission is the first ESA mission to Venus and will be launched in October 2005. Although it is a mission devoted to atmosphere observation, significant scientific return will be provided by the investigation of Venus surface using mainly the near-infrared imaging spectrometer (VIRTIS). Many key issues raised by the analysis of Magellan data on the surface characteristics and recent geological activity can be investigated by VIRTIS providing unique information on surface temperature, mineralogy, chemical weathering, recent volcanic activity and, eventually, earthquakes occurrence. Volcanism and tectonics strongly shaped the surface of Venus as revealed by the Magellan data. Large lowlands cover about 80% of the surface and highly deformed plateau (tesserae) form the highlands. Although there is evidence that majority of the observed tectonic and volcanic features of Venus formed in a short period of time close to 500 my ago, other volcanic and tectonic features appear to be formed in very recent time suggesting that the internal activity of the planet may be ongoing. The NIR wavelengths window will allow to penetrate the thick atmosphere and measure critical parameters of environmental condition (such as composition and redox state) to understand the weathering processes of the surface rocks and the identification of recent volcanic activity. The M channel of VIRTIS will allow the first systematic mapping of the surface and of the near-surface atmosphere of Venus in the near infrared wavelengths range. This will be done using the atmospheric windows located at 1.10, 1.18 ĉm and if possible also using the window at 1.02 ĉm. The latter is unfortunately right at the low end of the wavelength range of the IR channel and at the upper end of the VIS channel. Therefore the usability of this window is unclear until first data from Venus are obtained. The atmospheric windows will allow measuring the thermal emission of the surface as was demonstrated by Galileo/NIMS and Cassini/VIMS. Based on these data three main science tasks for the surface analysis will be pursued: Classification of the surface composition, study the interaction between low atmosphere and surface, and mapping of the variability of the surface temperature.
DE: 5464 Remote sensing
DE: 5494 Instruments and techniques
DE: 5499 General or miscellaneous
DE: 6295 Venus
SC: Planetary Sciences [P]
MN: Fall Meeting 2005