Venus spacecraft infrared radiance spectra and some aspects of their interpretation

Details Venus spacecraft infrared radiance spectra and some aspects of their interpretation Venus spacecraft infrared radiance spectra and some aspects of their interpretation

May 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apopt..25.1710m&link_type=abstract

Applied Optics (ISSN 0003-6935), vol. 25, May 15, 1986, p. 1710-1719.

Physics

Optics

19

Infrared Spectra, Satellite-Borne Instruments, Spectrometers, Venera Satellites, Venus (Planet), Abundance, Brightness Temperature, Emission Spectra, Fourier Transformation, High Resolution, Sulfur Dioxides, Thermal Radiation, Water

Scientific paper

Fourier spectrometers aboard the Venera 15 and 16 orbiters measured the outgoing spectral radiance of Venus in the 250-1600/cm and 400-1600/cm regions with a spectral resolution of 5-7/cm depending on the data handling procedure. This paper gives a short description of the experimental design and discusses those aspects that can be suitably tackled by wide range spectral measurements. Different Venusian regions can be characterized by typical and significantly different radiance and brightness temperature spectra based on the magnitude of brightness temperatures and also on secondary spectral signatures caused by H2SO4 bands as well as isotopic and hot CO2 bands. At least five groups can be identified, one typical for equatorial regions, one for midlatitudes, and three for the subpolar and polar regions. A detailed comparison between computed and measured spectra for the transition zone between midlatitudes and the cold subpolar region gives arguments that the cloud top is situated within the temperature inversion and not above or below it.

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