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Remote sensing of a comet at millimeter and submillimeter wavelengths from an orbiting spacecraft

dc.contributor.authorGULKIS, S.
dc.contributor.authorALLEN, M.
dc.contributor.authorBACKUS, C.
dc.contributor.authorBEAUDIN, Gérard
hal.structure.identifierLaboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA]
dc.contributor.authorBIVER, N.
hal.structure.identifierLaboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA]
dc.contributor.authorBOCKELEE-MORVAN, D.
hal.structure.identifierLaboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA]
dc.contributor.authorCROVISIER, J.
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorDESPOIS, D.
dc.contributor.authorENCRENAZ, P.
dc.contributor.authorFRERKING, M.
dc.date.issued2007
dc.identifier.issn0032-0633
dc.description.abstractEnThe ESA Rosetta Spacecraft, launched on March 2, 2004 with the ultimate destination being Comet 67P/Churyumov–Gerasimenko, carries a relatively small and lightweight millimeter–submillimeter spectrometer instrument, the first of its kind launched into deep space. The instrument, named Microwave Instrument for the Rosetta Orbiter (MIRO), consists of a 30-cm diameter, offset parabolic reflector telescope, which couples energy in the millimeter and submillimeter bands to two heterodyne receivers. Center-band operating frequencies are near 190 GHz (1.6 mm) and 562 GHz (0.5 mm). Broadband, total power continuum measurements can be made in both bands. A 4096-channel spectrometer with 44 kHz resolution is connected to the submillimeter receiver. The spectral resolution is sufficient to observe individual, thermally broadened spectral lines (T?10 K). The submillimeter radiometer/spectrometer is fixed tuned to measure four volatile species—CO, CH3OH, NH3 and three isotopes of water, H216O, H217O and H218O. The MIRO experiment will use these species as probes of the physical conditions within the nucleus and coma. The basic quantities measured by MIRO are surface temperature, gas production rates and relative abundances, and velocity and excitation temperature of each species, along with their spatial and temporal variability. This information will be used to infer coma structure and outgassing processes, including the nature of the nucleus/coma interface.
dc.language.isoen
dc.publisherElsevier
dc.subject.enComets
dc.subject.enSubmillimeter spectroscopy
dc.subject.enSpacecraft instruments
dc.title.enRemote sensing of a comet at millimeter and submillimeter wavelengths from an orbiting spacecraft
dc.typeArticle de revue
dc.identifier.doi10.1016/j.pss.2006.11.011
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
bordeaux.journalPlanetary and Space Science
bordeaux.page1050-1057
bordeaux.volume55
bordeaux.issue9
bordeaux.peerReviewedoui
hal.identifierhal-00157350
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00157350v1
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