Stratospheric thermal emission and absorption near the 22.235 Gc/s (1.35 cm) rotational line of water-vapour

Details Stratospheric thermal emission and absorption near the 22.235 Gc/s (1.35 cm) rotational line of water-vapour Stratospheric thermal emission and absorption near the 22.235 Gc/s (1.35 cm) rotational line of water-vapour

Feb 1965

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1965jatp...27..217c&link_type=abstract

Journal of Atmospheric and Terrestrial Physics, vol. 27, no. 2, pp. 217-233

Physics

5

Scientific paper

Following the suggestion of Barrett and Chung (1962) that the pressure-dependence of the strength and width of the 22.235 Gc/s (1.35 cm) water-vapour line might make it possible to detect water-vapour in the stratosphere from ground-based radiometer observations, the sky noise temperature spectrum resulting from this line has been calculated for a number of idealised stratospheric water-vapour distributions up to a height of 80 km, both for direct emission from the atmosphere and for atmospheric absorption of solar radiation. The calculations have been carried out for observation heights from 0 to 30 km, and, in the case of the absorption line, for solar zenith angles between 0° and 75°. Doppler broadening was found to be comparable with pressure-broadening above 70 km and was allowed for in the calculations. If the stratospheric water-vapour mixing ratio is independent of height then only the broad resonance due to water-vapour in the relativity high pressure tropospheric region will be seen, whereas if it increases appreciably with height then an enhancement at the centre of this broad resonance should be observed. If, for example, the stratospheric water-vapour density is independent of height and equal to 10-4 gm m-3, then a 3.5°K enhancement should be observed. The corresponding value for a density of 10-4 gm m-3, is 39°K. By using the sun as a source to observe the absorption line it should be possible to detect much smaller amounts of water-vapour in the stratosphere.

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