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At least 19 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1965

Lunar luminescence.

Lunar luminescence in vicinity of Aristarchus from 1783 to 1963, examining solar flare data

LUNAR LUMINESCENCE↗
NASA NTRS1966

Mechanisms for lunar luminescence.

Visibility of lunar luminescence, noting favorable possibilities at new Moon, dark eclipses and far side and energy sources for luminescence

LUNAR LUMINESCENCE↗
NASA NTRS1983

Lunar luminescence measurements

Spectra of lunar sites obtained in June 1983 have been analyzed for residual luminescence using the spectral line depth technique. The results or three sites each at three wavelengths are presented. The sites observed were Mare Crisium, Kepler, and Aristarchus. In each case, the value quoted was based not only on the strong Fraunhofer line in the spectral range covered but also on from 11 to 21 weaker lines within 80 A of the strongest feature. These data do not support previous observations. The values given do not indicate a greatly reddened spectrum, and the luminescence spectrum of the mare site is not significantly different from the two young crater sites. These observations cannot be adequately explained by thermal luminescence, theories of direct excitation are also unable to explain the strength of the flux.

Morgan, T. H.↗
NASA NTRS1984

Lunar luminescence and the filling-in of Fraunhofer lines in moonlight

The filling-in of Fraunhofer lines in moonlight has been attributed to lunar luminescence. In order to test mechanisms proposed for this effect, measurements were made of the filling-in of the H-alpha line, the Na D doublet, and a number of lines near the doublet. The degree of filling-in was not correlated with wavelength in a way expected from a broadband luminescence, such as thermoluminescence. However, it was correlated with equivalent width of the Fraunhofer line, such that it increased as equivalent width decreased. This suggests that the Fraunhofer line filling at the moon's surface is caused by inelastic scattering of sunlight with a small wavelength shift, as for example, photon-phonon scattering.

Potter, A. E.↗
NASA NTRS1970

Lunar luminescence and neutral particles

Luminescence of powdered silica and basalt bombarded by atomic hydrogen, relating spectral distributions dependence on ion energy to lunar luminescence

Anderson, D. L.↗
NASA NTRS1972

Luminescence analysis of lunar samples returned by Apollo: Luminescence of Apollo 14 and Apollo 15 lunar samples

Luminescence measurements were made of Apollo 14 lunar samples with far UV X-ray, and proton irradiation and of Apollo 15 lunar samples with X-ray irradiation. Preliminary efficiencies with the far UV are in the range 0.001 to 0.01; efficiencies with X-rays and protons are in the range 10 to the -8th to 10 to the -6th powers. The crystalline igneous rocks show higher efficiencies, in general, than the breccias and glasses, and the ratio of intensity of the green to the blue luminescence peak tends to be higher for the crystalline igneous rocks than for breccias and glasses. Therefore, both the efficiency and the spectral character appear to have a systematic relationship to lithologic type (granitic versus gabbroic versus fragmental) and to geologic history and processes on the moon (shocked versus unshocked or only mildly shocked material).

Greenman, N. N.↗
NASA NTRS1973

Experimental results on combined ultraviolet-proton excitation of moon rock luminescence.

The experimental results reported indicate that a small synergistic effect may exist between near-UV radiation and solar-wind-energy protons in solar radiation that could slightly enhance luminescence generation on the moon's surface. The magnitude of the effect, however, is far too small to account for the apparent orders-of-magnitude discrepancy between reported telescope measurements of lunar luminescence and the limitation of lunar luminescence intensity based on lab studies of moon rocks.

Nash, D. B.↗
NASA NTRS1972

Luminescence of Apollo 14 and Apollo 15 lunar samples.

Luminescence measurements have been made of Apollo 14 lunar samples with far UV, X-ray, and proton irradiation and of Apollo 15 lunar samples with X-ray irradiation. Preliminary efficiencies with the far UV are in the range .01 to .001; efficiencies with X-rays and protons are in the range .000001 to .00000001. The crystalline igneous rocks show higher efficiencies, in general, than the breccias and glasses, and the ratio of intensity of the green to the blue luminescence peak tends to be higher for the crystalline igneous rocks than for the breccias and glasses.

Greenman, N. N.↗