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Start Over Descriptor "1060)" Topic 0103 physical sciences
2 results on '"1060)"'

1. A latitudinal survey of CO, OCS, H2O, and SO2 in the lower atmosphere of Venus: Spectroscopic studies using VIRTIS-H

Author

P. Drossart, Florence Henry, Bruno Bézard, Emmanuel Marcq, Jean-Michel Reess, Giuseppe Piccioni, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
Atmospheric Science, Planetary Sciences: Solid Surface Planets: Composition (1060, 010504 meteorology & atmospheric sciences, Infrared, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Planetary Sciences: Solar System Objects: Venus, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Soil Science, Mineralogy, Venus, Aquatic Science, Oceanography, Atmospheric sciences, 01 natural sciences, Troposphere, Atmosphere, Atmosphere of Venus, chemistry.chemical_compound, Geochemistry and Petrology, 3672), 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Mixing ratio, Planetary Sciences: Solid Surface Planets: Atmospheres (0343, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth-Surface Processes, Water Science and Technology, Carbonyl sulfide, Ecology, biology, Paleontology, Forestry, biology.organism_classification, Planetary Sciences: Solid Surface Planets: Remote sensing, 1060), Geophysics, chemistry, 13. Climate action, Space and Planetary Science, Environmental science, Water vapor
Abstract

International audience; The high-resolution channel (R $\simeq$ 2000) of the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument (VIRTIS-H) aboard Venus Express has provided numerous spectra of the nightside infrared thermal emission in the 2.3-μm window. Mixing ratios of various minor species in the 30-40 km range could therefore be inferred using this spectral window at higher latitudes accessible to the spacecraft but which cannot be observed from Earth. The previously known enhancement in carbon monoxide (CO) toward high latitudes is confirmed and extended up to 60° with a mixing ratio varying from 24 +/- 3 to 31 +/- 2 ppmv at 36 km. Measurements of carbonyl sulfide (OCS) also agree with the previously suspected latitudinal variations that are anticorrelated with those of CO, ranging between 2.5 +/- 1 and 4 +/- 1 ppmv at 33 km. New constraints were also derived on the mean abundance of water vapor (H2O, 31 +/- 2 ppmv) and sulfur dioxide (SO2, 130 +/- 50 ppmv) in the probed altitude range. CO and OCS variations are interpreted as caused by large-scale vertical motions, an explanation under current testing by various chemical and dynamical modeling. In such a case, these variations may help constrain the chemical time scale of those species in the lower troposphere.

Published
2008
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2. Titan's inventory of organic surface materials

Author

Oded Aharonson, Stephen D. Wall, Bryan Stiles, Michael Janssen, Rosaly M. C. Lopes, Steven J. Ostro, Randolph L. Kirk, P. Paillou, Alexander G. Hayes, Jani Radebaugh, Jonathan I. Lunine, Ralph D. Lorenz, Giuseppe Mitri, Howard A. Zebker, Karl L. Mitchell, Ellen R. Stofan, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), US Geological Survey [Flagstaff], United States Geological Survey [Reston] (USGS), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Department of Electrical Engineering [Stanford], Stanford University, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Sciences et Technologies - Bordeaux 1, Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Geological Sciences [BYU], Brigham Young University (BYU), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, and Proxemy Research Inc

Subjects
Planetary Sciences: Solid Surface Planets: Surface materials and properties, 010504 meteorology & atmospheric sciences, Atmospheric sciences, 01 natural sciences, Methane, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], chemistry.chemical_compound, symbols.namesake, Impact crater, 0103 physical sciences, Planetary Sciences: Solid Surface Planets: Atmospheres (0343, Ejecta, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Hydrology, Life on Titan, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Atmospheric methane, Fossil fuel, Planetary Sciences: Solid Surface Planets: Remote sensing, Planetary Sciences: Solar System Objects: Titan, 1060), Geophysics, chemistry, 13. Climate action, Greenhouse gas, symbols, General Earth and Planetary Sciences, Titan (rocket family), business, Geology
Abstract

[1] Cassini RADAR observations now permit an initial assessment of the inventory of two classes, presumed to be organic, of Titan surface materials: polar lake liquids and equatorial dune sands. Several hundred lakes or seas have been observed, of which dozens are each estimated to contain more hydrocarbon liquid than the entire known oil and gas reserves on Earth. Dark dunes cover some 20% of Titan's surface, and comprise a volume of material several hundred times larger than Earth's coal reserves. Overall, however, the identified surface inventories (>3 × 104 km3 of liquid, and >2 × 105 km3 of dune sands) are small compared with estimated photochemical production on Titan over the age of the solar system. The sand volume is too large to be accounted for simply by erosion in observed river channels or ejecta from observed impact craters. The lakes are adequate in extent to buffer atmospheric methane against photolysis in the short term, but do not contain enough methane to sustain the atmosphere over geologic time. Unless frequent resupply from the interior buffers this greenhouse gas at exactly the right rate, dramatic climate change on Titan is likely in its past, present and future.

Published
2008
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