Cloud structure in Venus middle-to-lower atmosphere as inferred from VEX/VIRTIS 1.74 μm data

T. Satoh, T. Imamura, Joji Hashimoto, N. Iwagami, K. Mitsuyama, S. Sorahana, P. Drossart, G. Piccioni

Research output: Contribution to journalArticle

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Abstract

We have analyzed 1.74 μm nightside emission of Venus recorded using Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) onboard European. Space Agency's (ESA) Venus Express (Orbit 344, 30-31 March 2007). Attention was paid to how infrared radiance, intense at the center of the 1.74 μm "window", dims at an off-center wavelength (1.71 μm). Cloud models are required to simultaneously reproduce the emission intensity at 1.74 μm and the ratio of intensities (I1.71μm/I1.71μm)- Our best-fit model (5 km vertical resolution.) has located the main cloud opacity in 40-45 km altitude, lower than previous studies. This may be due to the use of CO2 line parameters from a relatively new source (Carbon Dioxide Spectroscopy Databank) which may also be responsible for weaker continuum absorption 5.6 × 10-9 cm-1 amagat-2 The data are reproduced well by models of which total aerosol optical thickness is 30-50 plus subcloud haze at 30-40 km altitude. We have mapped the subcloud haze opacity (approximately 0-4) and found that the opacity basically anticorrelates with the 1.74 μm intensity. There are regions of "positive" correlation which may imply enhanced production of aerosols due to penetration of more sunlight in less cloudier regions. Venus Express, now with a capability of sensing "from the top to the bottom" of Venus cloud system, will greatly enhance our knowledge about the current status of Venus atmosphere.

Original languageEnglish
Article numberE00B37
JournalJournal of Geophysical Research B: Solid Earth
Volume114
Issue number4
DOIs
Publication statusPublished - Apr 20 2009
Externally publishedYes

Fingerprint

lower atmosphere
imaging spectrometers
Venus (planet)
Opacity
Infrared imaging
Venus
opacity
Spectrometers
spectrometer
haze
Aerosols
atmosphere
aerosols
Venus clouds
Venus atmosphere
low altitude
sunlight
European Space Agency
radiance
Carbon Dioxide

ASJC Scopus subject areas

  • Geochemistry and Petrology
  • Geophysics
  • Earth and Planetary Sciences (miscellaneous)
  • Space and Planetary Science

Cite this

Cloud structure in Venus middle-to-lower atmosphere as inferred from VEX/VIRTIS 1.74 μm data. / Satoh, T.; Imamura, T.; Hashimoto, Joji; Iwagami, N.; Mitsuyama, K.; Sorahana, S.; Drossart, P.; Piccioni, G.

In: Journal of Geophysical Research B: Solid Earth, Vol. 114, No. 4, E00B37, 20.04.2009.

Research output: Contribution to journalArticle

Satoh, T. ; Imamura, T. ; Hashimoto, Joji ; Iwagami, N. ; Mitsuyama, K. ; Sorahana, S. ; Drossart, P. ; Piccioni, G. / Cloud structure in Venus middle-to-lower atmosphere as inferred from VEX/VIRTIS 1.74 μm data. In: Journal of Geophysical Research B: Solid Earth. 2009 ; Vol. 114, No. 4.
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