Venusian atmospheric turbulence evaluated from cloud brightness distribution in VEX UV images

Details Venusian atmospheric turbulence evaluated from cloud brightness distribution in VEX UV images Venusian atmospheric turbulence evaluated from cloud brightness distribution in VEX UV images

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf...48t&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.48

Astronomy and Astrophysics

Astronomy

Scientific paper

This study suggested following points: (1) The power spectra mostly contained the inflection. The slope at lower wavenumbers was steeper than that at higher wavenumbers. Such a feature agrees with the characteristics in the kinetic energy spectra shon Earth (Nastrom et al., 1984; Nastrom and Gage, 1985). (2) The slopes at planetary wavenumbers K < 50 (0.001 /km at the latitude of 20S) had intermediate value between the theoretical ones, -3 and -5/3. It agrees well with the previous Venusian studies (e.g. Peralta et al., 2007). This feature was common over three years. (3) We first derived the slope at higher wavenumbers, 0.002 - 0.01 /km, which was due to the high spatial resolution of VMC. However, it was sometimes close to 0, which might be affected by instrumental noise. We are doing further checks. (4) We found some temporal and spatial changes of the slopes in short interval as several hours. This result also suggests that the PSD slope has a large variability in the individual latitude. (5) The wavenumbers at the inflection point were 0.001 - 0.003 /km. Kitamura and Matsuda (2006) suggested that the inflection point at 330 - 1000km can be a border between 2D and 3D turbulences. Our result indicates a possibility to have enstrophy forward cascade in 2D turbulence at lower wavenumbers and the energy forward cascade in 3D turbulence at higher wavenumbers.

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