Felsic highland crust on Venus suggested by Galileo Near‐Infrared Mapping Spectrometer data

DOI Web Site Web Site 被引用文献9件 オープンアクセス
  • George L. Hashimoto
    Laboratory for Earth and Planetary Atmospheric Science Organization of Advanced Science and Technology, Kobe University Kobe Japan
  • Maarten Roos‐Serote
    Lisbon Astronomical Observatory Lisbon Portugal
  • Seiji Sugita
    Department of Complexity Science and Engineering Graduate School of Frontier Science, University of Tokyo Kashiwa Japan
  • Martha S. Gilmore
    Department of Earth and Environmental Sciences Wesleyan University Middletown Connecticut USA
  • Lucas W. Kamp
    Jet Propulsion Laboratory California Institute of Technology Pasadena California USA
  • Robert W. Carlson
    Jet Propulsion Laboratory California Institute of Technology Pasadena California USA
  • Kevin H. Baines
    Jet Propulsion Laboratory California Institute of Technology Pasadena California USA

書誌事項

公開日
2008-05
権利情報
  • http://onlinelibrary.wiley.com/termsAndConditions#vor
DOI
  • 10.1029/2008je003134
公開者
American Geophysical Union (AGU)

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説明

<jats:p>We evaluated the spatial variation of Venusian surface emissivity at 1.18 <jats:italic>μ</jats:italic>m wavelength and that of near‐surface atmospheric temperature using multispectral images obtained by the Near‐Infrared Mapping Spectrometer (NIMS) on board the Galileo spacecraft. The Galileo NIMS observed the nightside thermal emission from the surface and the deep atmosphere of Venus, which is attenuated by scattering from the overlying clouds. To analyze the NIMS data, we used a radiative transfer model based on the adding method. Although there is still an uncertainty in the results owing to the not well known parameters of the atmosphere, our analysis revealed that the horizontal temperature variation in the near‐surface atmosphere is no more than ±2 K on the Venusian nightside and also suggests that the majority of lowlands likely has higher emissivity compared to the majority of highlands. One interpretation for the latter result is that highland materials are generally composed of felsic rocks. Since formation of a large body of granitic magmas requires water, the presence of granitic terrains would imply that Venus may have had an ocean and a mechanism to recycle water into the mantle in the past.</jats:p>

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