Search

High-resolution ground-based solar spectra recorded at the Amundsen-Scott South Pole station in Dec. 1980 and Nov. 1986 have been analyzed in the region of the CF(2)Cl(2) (chlorofluorocarbon 12) nu(8) band Q branches at 1161 cm(-1). An increase in the CF(2)Cl(2) total vertical column above the South Pole of 1.24 +/- 0.15 over the 6-yr period, corresponding to an average rate of increase of 3.6 +/- 2.1%, is derived. This rate of increase is lower than indicated by in situ measurements at the South Pole over the same time period, but there is agreement when the rather error bars of the spectral measurement results are considered. Spectroscopic parameters that can successfully model CF(2)C1(2) absorption at low temperatures are needed to improve retrieval accuracies and could be applied to a number of pre-1980 atmospheric spectral data sets in the literature to obtain an improved record of early CF(2)Cl(2) concentration trends for comparison with estimates of historical release rates.

The stratospheric water vapor mixing ratio altitude profile has been derived from spectral observations of the downward night emission from the pure rotation water vapor lines in the 24-29-microm region of the spectrum. The data were obtained during two balloon flights, made on 22 February 1971 and on 29 June 1971, using a balloon-borne spectral radiometer with ~2 cm(-1) resolution. The observed radiances have been fitted to line-by-line, layer-by-layer radiance calculations, from which the water vapor mixing ratio between 10 km and 30 km has been flights show a broad minimum around of 6 x 10(-7)g/g to 4 x 10(-6) g/g.

A grating spectrometer with a Ge: Cu detector was flown on three balloon flights. Spectra in the 4-14.3-micro region were obtained at various altitudes from the ground through 30 km with a resolution considerably better than that achieved in previous flights. Some of the spectra were obtained over long paths at float altitude, during the sunset. Data from these flights are presented with a discussion of the significant features of the observed absorptions. Special emphasis is put on the new features observed during the sunset.

A balloon-borne spectrometer was used to measure the atmospheric absorption of solar radiation in the 9-10-micro region as a function of altitude. Among the numerous spectra recorded, several were made with very long optical paths above the troposphere obtained from floating altitude (~30 km) while the sun set. When the experimental results are compared with calculated spectra, based on line by line parameters of the nu(3) and nu(1) fundamentals of ordinary ozone, (16)O(3), combined with the Curtis-Godson approximation, large discrepancies are found for the long path spectra. It is shown that the hot bands nu(3), + nu(2), - nu(2), and nu(3), + nu(3), - nu(3), of the (16)O(3), and the nu(3) fundamentals of the isotopic species (16)O(18)O(16)O and (16)O(16)O(18)O, can contribute significant absorption for long paths such as obtained in this experiment. Such long paths also give rise to significant absorptions by the nu(3) - nu(1) and the nu(3) - 2nu(2) degrees bands of CO(2). Including these weak bands in the calculated spectra leads to good agreement with the observed data.

A balloon-borne, 0.5-m, Czerny-Turner grating spectrometer has been designed and constructed at the University of Denver and has measured atmospheric transmittance in several spectral regions between 2 micro and 14 micro. These data have been obtained on a series of eleven balloon flights at three geographic locations over a period of thirty months. The solar pointing system, spectrometer optics, electronics and recording system are described. The preflight and flight performance of the spectrometer is discussed and sample data presented.