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Results for “MICHELSON INTERFEROMETERS”

Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

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At least 127 records · Page 7
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NASA NTRS1970

Infrared spectra for 32 stars

Stellar IR spectra for types A0 to M7, using Mertz type Michelson interferometer as Fourier transform spectrometer

Johnson, H. L.↗
NASA NTRS1971

Vibration testing and analysis using holography

Time average holography is useful in recording steady state vibrational mode patterns. Phase relationships under steady state conditions are measured with real time holography and special phase shifting techniques. Data from Michelson interferometer verify vibration amplitudes from holographic data.

Source record↗
NASA NTRS1971

Vertical sounding of the atmosphere with the Nimbus IV infrared spectrometer experiment.

Nimbus III and IV meteorological satellite data obtained on a Michelson interferometer are used as a basis for sounding the vertical temperature and water-vapor and ozone content profiles in the atmosphere. Selection of suitable locations and bandwidths for making such soundings efficient is discussed. Several transmittance models of the atmosphere, and terrain properties and cloud emissivity effects as factors influencing the sounding results are considered.

Conrath, B. J.↗
NASA NTRS1973

Infrared spectra of the Galilean satellites of Jupiter.

Spectra of the four Galilean satellites from 1 to 4 microns were obtained with a Michelson interferometer. The spectra show that the albedo of Io is quite flat and shows no absorptions in the region observed. Europa and Ganymede have large amounts of water ice on their surface. Callisto shows some faint ice absorptions. Upper limits of 0.5 cm-atm (STP) corresponding to .00000006 atm partial surface pressure were set for CH4 and NH3 on all four satellites.

Fink, U.↗
NASA NTRS1973

Infrared spectra of the Galilean satellites of Jupiter

Spectra of the four Galilean satellites from 1 to 4 microns were obtained with a Michelson interferometer. The spectra show that the albedo of Io is very nearly constant with wavelength; no absorptions are found in the region observed. Europa and Ganymede have large amounts of water ice on their surface. Callisto shows some faint ice absorptions. Upper limits of 0.5 cm-atm (STP) corresponding to 6 x 10 to the minus 8th power atm partial surface pressure were set for CH4 and NH3 on all four satellites.

Fink, U.↗
NASA NTRS1973

Spectral reflectance and emittance of particulate materials. I - Theory. II - Application and results

The sizes, shapes, and complex refractive indices of particles are calculated in a study of the IR spectral reflectance of a semiinfinite medium composed of irregular particles of different materials. Geometric optics techniques with corrections for additional absorption due to particle edges and asperities is used in scattering and absorption calculations for particles larger than the wavelength. A Lorentz-Lorenz model is used to derive the averaged complex index of the medium, assuming that its individual particles are ellipsoids. Experimental results obtained on a Michelson interferometer for the spectral emittance of particulate mineral materials are compared with theoretical results. Good agreement between the experimental and theoretical results suggests the applicability, in remote IR spectroscopy, of the theoretical concepts applied in this study.

Emslie, A. G.↗
NASA NTRS1974

Balloon-based measurements of the cosmic background radiation

A balloon-borne liquid-helium-cooled spectrometer was developed and flown to measure the cosmic background radiation in the 3- to 18-per-cm region. It features a cooled horn antenna, a polarizing Michelson interferometer, and a germanium bolometer. These design features and the performance of the instrument are discussed.

Mather, J. C.↗
NASA NTRS1975

Water vapor absorption spectra of the upper atmosphere /45-185 per cm/

The far IR nighttime absorption spectrum of the earth's atmosphere above 14 km is determined from observations of the bright moon. The spectra were obtained using a Michelson interferometer attached to a 30-cm telescope aboard a high-altitude jet aircraft. Comparison with a single-layer model atmosphere implies a vertical column of 3.4 plus or minus 0.4 microns of precipitable water on 30 August 1971 and 2.4 plus or minus 0.3 microns of precipitable water on 6 January 1972.-

Augason, G. C.↗