Centimeter emission variation of Venus: Its second phase

Details Centimeter emission variation of Venus: Its second phase Centimeter emission variation of Venus: Its second phase

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ipesprept.....f&link_type=abstract

M.S. Thesis, 2 Oct. 1989 Instituto de Pesquisas Espaciais, Sao Jose dos Campos (Brazil).

Physics

Brightness Temperature, Periodic Variations, Phase Shift, Radio Emission, Venus (Planet), Planetary Temperature, Sulfur Dioxides, Sulfuric Acid, Water

Scientific paper

The radio emission from the planet Venus, at wavelengths smaller than 10 centimeters, presents some fluctuations in the brightness temperature. The reasons for those fluctuations are still inconclusive. During 1988, Venus was relatively closer to the Earth than in the preceeding years and also presented large phase angle changes along the year. This exceptional orbital configuration allowed to program an extensive series of observations with the scope of finding out if there is any fluctuation in the planetary brightness temperature associated to its phase. For this program the 13.7 m antenna of the Itapetinga Radio Observatory was used, the observations being carried out in 22 GHz and 43 GHz. The observational results of Venus brightness temperature, from March to October 1988, which shows some fluctuations in this temperature are presented. The results of observations suggest that the variation of the brightness temperature is probably due to the phase angle of the planet. This temperature variation may be due to variations in the abundance of SO2, H2O, and gaseous H2SO4 which are the main absorbers in those wavelengths.

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