The upper clouds of Venus: Determination of the scale height from NIMS-Galileo infrared data

Details The upper clouds of Venus: Determination of the scale height from NIMS-Galileo infrared data The upper clouds of Venus: Determination of the scale height from NIMS-Galileo infrared data

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993p%26ss...41..505r&link_type=abstract

Planetary and Space Science (ISSN 0032-0633), vol. 41, no. 7, p. 505-514

Astronomy and Astrophysics

Astronomy

14

Brightness Temperature, Infrared Spectra, Limb Darkening, Near Infrared Radiation, Scale Height, Temperature Profiles, Venus (Planet), Venus Clouds, Astronomical Spectroscopy, Galileo Spacecraft, Infrared Spectroscopy, Pioneer Venus Spacecraft, Spaceborne Astronomy

Scientific paper

The 3-5 micrometer thermal emission of the nightside of Venus, recorded by the Near-Infrared Mapping Spectrometer (NIMS) instrument at the time of the Galileo flyby of Venus, is analysed to infer the properties of the upper cloud boundary. From the global maps of Venus at fixed wavelengths, the limb darkening of the flux is measured at several latitudes, within each infrared channel. By using the nominal Pioneer Venus thermal profile, these data give access to two parameters: the cloud deck temperature and the cloud scale height. It is verified independently, from the NIMS spectra, that this thermal profile is consistent with all the NIMS observations, and that the thermal structure does not vary significantly in the latitude range (25 deg S, 30 deg N). Within this range, the cloud scale height is found to be constant with latitude, and is H = 5.2 km, with an accuracy of about 15%, taking into account the various sources of theoretical and observational uncertainties. At higher latitudes, the temperature profile becomes more isothermal and the presented method to retrieve H is no longer valid.

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