Middle Ultraviolet Research Articles

Optically Contacted, Fabry-Perot Interferometer Filter for the Middle Ultraviolet

Get PDF Email Share Share with Facebook Tweet This Post on reddit Share with LinkedIn Add to CiteULike Add to Mendeley Add to BibSonomy Get Citation Copy Citation Text B. Bates, J. K. Conway, C. D. McKeith, and H. W. Yates, "Optically Contacted, Fabry-Perot Interferometer Filter for the Middle Ultraviolet," Appl. Opt. 12, 140-142 (1973) Export Citation BibTex Endnote (RIS) HTML Plain Text Citation alert Save article

Atmospheric Scattering of the Solar Flux in the Middle Ultraviolet

Spectra in the middle uv obtained on a rocket flight by a spectrometer pointed downward at the earth are compared with synthetic spectra generated by a computer. The independent variables of the synthetic spectra are the altitude of the detector, the wavelength, the zenith angles of the sun and of the detector line-of-sight, the azimuth difference between them, and three parameters characterizing the ozone distribution. In the altitude range of primary interest only two of the ozone parameters are free. Taken into account are the roundness of the earth, first-order Rayleigh scattering by the atmosphere, attenuation by air, absorption by molecular oxygen and ozone, and the line structure in the solar spectrum. The effects on the synthetic spectra of varying the parameters of the ozone distribution and the geometric parameters are also studied.

Attenuation by Ozone and the Earth’s Albedo in the Middle Ultraviolet

An approximate analytical expression is developed for the attenuation of middle ultraviolet radiation along slant paths through the atmosphere. The independent variables are wavelength, altitude of source (the detector is assumed to be above the atmosphere), angle of path with respect to zenith, and three parameters which characterize the ozone distribution. An approximate analytical expression is also developed for the scattered solar radiance seen by a satellite. Here the independent variables are the wavelength, the look angle and the sun angle with respect to the zenith, the scattering angle, and again three parameters which characterize the ozone distribution. The results based upon the formula are compared with previous studies and an experimental measurement.

Stellar Flux Measurements in the Middle Ultraviolet.

view Abstract Citations (1) References Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Stellar Flux Measurements in the Middle Ultraviolet. Boggess, Albert, III Abstract The program of rocket- based broad-bandpass stellar photometry at ultraviolet wavelengths is being continued. Small photometers are employed using combination interference and crystal filters which isolate 250-A bands centered at 2600 and 2200 A. A band at 2700 A is used as a control to compare the present data with those previously obtained at the latter wavelength (Boggess and Dunkelman 1958). Absolute fluxes have been obtained with an accuracy of about 20%, and when these data are combined with ground observation, colors below and spanning the Balmer discontinuity may be formed for comparison with conventional visual color data. Publication: The Astronomical Journal Pub Date: March 1961 DOI: 10.1086/108543 Bibcode: 1961AJ.....66R.279B full text sources ADS |