The moon - Mid-infrared (7.5- to 11.4-microns) spectroscopy of selected regions

Details The moon - Mid-infrared (7.5- to 11.4-microns) spectroscopy of selected regions The moon - Mid-infrared (7.5- to 11.4-microns) spectroscopy of selected regions

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992icar..100...73s&link_type=abstract

Icarus (ISSN 0019-1035), vol. 100, no. 1, p. 73-84.

Astronomy and Astrophysics

Astronomy

18

Astronomical Spectroscopy, Infrared Astronomy, Infrared Spectroscopy, Near Infrared Radiation, Basalt, Lunar Craters, Lunar Maria, Lunar Surface

Scientific paper

Scaled spectral emissivity spectra have been obtained from five locations on the illuminated lunar surface and are interpreted in terms of differences in their mineralogic composition. The emission maximum, which typically falls near 8.0 microns for lunar rocks and fines, is observed to be shifted from 7.9 microns for noritic Copernicus crater walls to 8.1 microns for the olivine-rich central peak. Two mare locations show the emission maximum centered at 8.0 microns, consistent with laboratory emission measurements of basalts. An emissivity minimum at 10.5 microns in the spectrum from central peak 2 is attributed to the presence of olivine. Minima centered at 8.75 microns in the crater wall spectra resemble minima in laboratory spectra from pyroxene. A broad minimum centered at 8.5 microns in the Kepler ejecta spectrum and a sharp drop in emissivity at wavelengths longer than 11 microns in spectra from both mare locations suggest plagioclase.

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