Abstract
Optical remote sensing of the atmosphere in its most elementary form is visual observation of clouds, haze, and wind. Early solar spectroscopists observed that the apparent solar spectrum recorded with the sun near the horizon contains many more absorption lines than does the apparent solar spectrum contain recorded when the sun is near the zenith. These new absorption lines were recognized to be signatures of molecules in the atmosphere. Later instruments to measure linear polarization, intensity fluctuations, intensity, and spectra as a function of scattering angle were used to reveal properties of small particles suspended and blown around within the atmosphere.
© 1983 Optical Society of America
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