Investigation of the thermal structure of the upper atmosphere of Venus by 10 micron heterodyne spectroscopy

Details Investigation of the thermal structure of the upper atmosphere of Venus by 10 micron heterodyne spectroscopy Investigation of the thermal structure of the upper atmosphere of Venus by 10 micron heterodyne spectroscopy

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985infph..25..505k&link_type=abstract

(European Physical Society, International Conference on Infrared Physics, 3rd, Zurich, Switzerland, July 23-27, 1984) Infrared P

Physics

Optics

1

Astronomical Spectroscopy, Infrared Spectroscopy, Line Spectra, Optical Heterodyning, Venus Atmosphere, Carbon Dioxide Lasers, Cassegrain Optics, Spectral Resolution, Venus, Thermal Properties, Structure, Atmosphere, Spectroscopy, Spectra, Kinetics, Rotation, Temperature, Altitude, Comparisons, Perturbations, Probes, Clouds, Layers, Pressure

Scientific paper

The Venusian atmosphere has been investigated using a 10 μm heterodyne spectrometer (spectral resolution λ/Δλ = 3×106) during upper conjunction and during elongation in 1983. In both cases a variety of spectra from the subsolar region were taken with high spatial resolution showing fully-resolved lines of the 10 μm laser transition of CO2. From these measurements kinetic and rotational temperatures are derived (T ≡ 200K). These spectroscopically-derived temperatures represent the atmospheric temperature for extended areas (1000 - 6000 km dia) at an altitude of 100 - 120 km. They are in agreement with on-the-spot temperature measurements indirectly obtained by space probes during descent. Multiple-line structures have been observed in the 10 μm spectra, which indicate a wave-like perturbation on the vertical temperature profile above a cloud layer at ≡20 mb atmospheric pressure.

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