Radiative Effects on the Formation of the Stably Stratified Layer in the Lower Atmosphere of Venus

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  • TAKAHASHI Yoshiyuki O.
    Department of Planetology, Kobe University, Kobe, Japan Center for Planetary Science, Kobe University, Kobe, Japan
  • HAYASHI Yoshi-Yuki
    Department of Planetology, Kobe University, Kobe, Japan Center for Planetary Science, Kobe University, Kobe, Japan
  • HASHIMOTO George L.
    Department of Earth Sciences, Okayama University, Okayama, Japan
  • KURAMOTO Kiyoshi
    Department of Cosmosciences, Hokkaido University, Hokkaido, Japan
  • ISHIWATARI Masaki
    Department of Cosmosciences, Hokkaido University, Hokkaido, Japan
  • KASHIMURA Hiroki
    Department of Planetology, Kobe University, Kobe, Japan Center for Planetary Science, Kobe University, Kobe, Japan

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<p>The formation of the stable layer below about 2 × 106 Pa pressure level (about 20 km altitude) of the atmosphere of Venus detected by in situ observations is investigated by the use of a radiative-convective equilibrium model. We demonstrate that, assuming mixing ratio profiles of absorbers to be at the upper limits of the observed ranges for H2O and SO2 and the lower limit for CO, a stable layer forms as a radiative-convective equilibrium state, but its stability is lower than the observed one. Also, increasing the continuum absorption coefficient of CO2 and/or H2O, which are not well constrained observationally or experimentally, results in the formation of a stable layer whose stability is comparable to the observed one. These results suggest a practical method to form the stable layer in the dynamical models of the Venus atmosphere. Further, these results indicate that the important targets of future observations and laboratory measurements are to obtain more precise profiles of the mixing ratios of H2O, CO, and SO2 in the Venus atmosphere, and to determine the continuum absorption coefficients of those.</p>

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