Cloud top structure of Venus revealed by Subaru/COMICS mid-infrared images

T. M. Sato, H. Sagawa, T. Kouyama, K. Mitsuyama, T. Satoh, S. Ohtsuki, M. Ueno, Y. Kasaba, M. Nakamura, T. Imamura

Research output: Contribution to journalArticlepeer-review

11 Citations (Scopus)

Abstract

We have investigated the cloud top structure of Venus by analyzing ground-based images taken at the mid-infrared wavelengths of 8.66. μm and 11.34. μm. Venus at a solar phase angle of ~90°, with the morning terminator in view, was observed by the Cooled Mid-Infrared Camera and Spectrometer (COMICS), mounted on the 8.2-m Subaru Telescope, during the period October 25-29, 2007. The disk-averaged brightness temperatures for the observation period are ~230. K and ~238. K at 8.66. μm and 11.34. μm, respectively. The obtained images with good signal-to-noise ratio and with high spatial resolution (~200. km at the sub-observer point) provide several important findings. First, we present observational evidence, for the first time, of the possibility that the westward rotation of the polar features (the hot polar spots and the surrounding cold collars) is synchronized between the northern and southern hemispheres. Second, after high-pass filtering, the images reveal that streaks and mottled and patchy patterns are distributed over the entire disk, with typical amplitudes of ~0.5. K, and vary from day to day. The detected features, some of which are similar to those seen in past UV images, result from inhomogeneities of both the temperature and the cloud top altitude. Third, the equatorial center-to-limb variations of brightness temperatures have a systematic day-night asymmetry, except those on October 25, that the dayside brightness temperatures are higher than the nightside brightness temperatures by 0-4. K under the same viewing geometry. Such asymmetry would be caused by the propagation of the migrating semidiurnal tide. Finally, by applying the lapse rates deduced from previous studies, we demonstrate that the equatorial center-to-limb curves in the two spectral channels give access to two parameters: the cloud scale height H and the cloud top altitude zc. The acceptable models for data on October 25 are obtained at H=. 2.4-4.3. km and zc=. 66-69. km; this supports previous results determined from spacecraft observations.

Original languageEnglish
Pages (from-to)386-399
Number of pages14
JournalIcarus
Volume243
DOIs
Publication statusPublished - 2014

Keywords

  • Atmospheres, dynamics
  • Atmospheres, structure
  • Infrared observations
  • Radiative transfer
  • Venus, atmosphere

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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