Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.2230d&link_type=abstract
American Astronomical Society, DPS meeting #28, #22.30; Bulletin of the American Astronomical Society, Vol. 28, p.1147
Astronomy and Astrophysics
Astronomy
Scientific paper
High resolution spectra of Jupiter at 5 mu m (resolving power of 10,000) have been obtained with the Fourier Transform Spectrometer at Canada-France-Hawaii Telescope during the nights of July 29--31, 1996. The following regions have been observed with a 2.5-arcsec aperture: the Great Red Spot and vicinity, three different 5-mu m hot spots of the North Equatorial Belt at 6.5deg N, and the Northern latitudes at 60deg N. The GRS and one of the hot spots were the targets of the Galileo/NIMS observations in the first orbit (Carlson et al., DPS-96), and the combination of the NIMS high spatial resolution spectral images with the FTS high spectral resolution observations will give important constraints on the tropospheric structure and composition of Jupiter. The 5-mu m spectrum of Jupiter is sensitive to the deep (2--8 bars) atmospheric structure, in particular to an intermediate cloud located between 1.5 and 2 bars, (Drossart et al., Icarus, 1982), probably the cloud observed by the Galileo Probe nephelometer at 1.55 bar (Ragent et al., Science, 1996). The domain from 4.59 to 4.81 mu m which has been covered, includes the spectral tropospheric absorption features of GeH_4, PH_3, AsH_3 and CH_3D. The atmospheric and cloud structures are both affecting the shape of the spectrum, and these observations give some constraints on the structure of the atmosphere in the observed atmospheric features. In the Northern latitudes, the absorption by AsH_3 is stongly enhanced, more than can be accounted for by emission angle dependence, which suggests an enhancement of AsH_3 in the high latitudes. A similar enhancement in phosphine had been observed in the Northern latitudes (Drossart et al., Icarus, 1990). Such variations could be due to deep convection latitudinal variability, or to a lower photochemical destruction of these compounds at high latitudes. (*) Visiting Astronomer at the Canada-France-Hawaii Telescope, which is operated by the Canadian National Research Council, the french Centre National de la Recherche Scientifique and the Univeristy of Hawaii.
Bezard Bruno
Drossart Pierre
Encrenaz Th.
Lellouch Emmanuel
Maillard Jean Pierre
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