Other
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.5304b&link_type=abstract
American Astronomical Society, DPS meeting #40, #53.04; Bulletin of the American Astronomical Society, Vol. 40, p.494
Other
Scientific paper
The analysis of the brightness spectral distribution of the fully cloud covered atmosphere of Jupiter provides an essential information on the characteristic spatial scales of atmospheric features and their distribution. As previously proposed by other authors, the analysis of the brightness power spectra can be used as an approximation to the kinetic energy spectrum of the planet, and therefore they can be representative of the turbulent regime of the planet. For this aim, we have used HST (1995) and Cassini's ISS (2000) observations in the near-infrared ( 950 nm, NIR), blue (430 nm, BL) and ultraviolet ( 260 nm, UV) wavelengths. The images were cylindrically projected and corrected from limb-darkening to obtain planispheres extending approximately from -60º to +60º planetocentric latitude. We retrieved zonal albedo scans each 0.1º in latitude and determine corresponding power spectra by means of a Fast Fourier Transform. Similarly, we also computed mean meridional brightness scans for a meridional analysis. For the zonal analysis, we found two slope ranges, n1 = -1.3 ± 0.4 for wavenumbers between 10 and 80 and n2 = -2.5 ± 0.7 between 80 and 150 in NIR and BL. In UV observations, we got n1 = 1.9 ± 0.4 and n2 = -0.7 ± 0.4 in UV. The meridional analysis is in excellent agreement with previous works based on mean zonal wind profiles with a slope of -5 for the NIR and BL wavelengths but not for the UV. All these results are discussed in terms of the two-dimensional turbulence theory and of the characteristic dynamic scales of the planet.
Barrado-Izagirre Naiara
Perez-Hoyos Santiago
Sanchez-Lavega Agustín.
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