Cloud altitudes of Jupiter estimated by imaging observation using a liquid crystal variable filter in the 650 - 1000 nm spectral range

Details Cloud altitudes of Jupiter estimated by imaging observation using a liquid crystal variable filter in the 650 - 1000 nm spectral range Cloud altitudes of Jupiter estimated by imaging observation using a liquid crystal variable filter in the 650 - 1000 nm spectral range

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005dps....37.3031m&link_type=abstract

American Astronomical Society, DPS meeting #37, #30.31; Bulletin of the American Astronomical Society, Vol. 37, p.1565

Astronomy and Astrophysics

Astronomy

Scientific paper

A large optical depth of clouds obstructs us to observe the movement of the atmosphere under clouds directly. However, we can investigate dynamics of the atmosphere indirectly, if we get information on rugged cloud top. To take Jupiter's images at a number of wavelengths and to obtain the spectra of atmosphere at absorption bands of methane make it possible to reproduce three-dimensional structure of cloud top and haze precisely. Using a liquid crystal variable filter (CRI, FWHM 10 nm), a visible and near-infrared reflecting 60 cm telescope, and a cooled CCD camera (PixelVision, 652x494 pixels), we obtained the images of Jupiter at 71 wavelengths in the range of 650 - 1000 nm in 10 minutes on April 14, 2005 at Iitate observatory, Fukushima, Japan. We got spectra of atmosphere at each region of Jupiter's disk. To correct absorption effect due to the atmosphere of the Earth and the spectral characteristics of the instruments in wavelength, we observed some standard stars in the same operation mode. We determined the altitudes of ammonia clouds over entire Jupiter's disk based on the calculation of spectral features fitted to the observation results at absorption bands of methane. We used a radiative transfer equation, considering the effects of Rayleigh scattering, the absorption of methane, thick ammonia clouds, and the pressure and temperature profile measured by the Galileo Probe. Although EZ (Equatorial Zone) is higher altitude cloud than NEB (North Equatorial Belt), the observed spectra of EZ show stronger absorption than that of NEB at ammonia absorption bands(790, 930 nm). This fact suggests that the column density of ammonia above EZ is larger than that above NEB.

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