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• W1530352014 abstract "Abstract Spectra of the Moon in the range 2-15μ have been obtained with the help of the infrared telescope-spectrometer aboard Saljut 5. They have been compared with the spectra of regolith returned by Luna 24. The reflected intensity is greatest in the range from 3 to 5μ (up to 60% for Saljut 5 and 30% for Luna 24), while at 11.5μ the intensity is reduced. From Luna 24, water absorption bands appear in the spectra at certain depths in the core; the concentration of water is estimated to be 0.1%. The spectrum of the Moon between 2 and 7μ was first obtained in 1975, enabling some preliminary conclusions to be made about the reflection characteristics of the Moon (1). The radiation spectra of the Moon obtained from Saljut 5 between 1.6 and 15μ as well as the spectral data for the soil samples from Luna 24, which have a higher accuracy that previous ones such as Luna 16, Apollo 11, etc. (2), show a number of important new properties. The telescope-spectrometer of Saljut 5 automatically recorded the radiation spectrum of the Moon on November 5, 1976, at 9 h 54 m U.T. on orbit 2180, and on December 7, 1976, at 22 h 146 m U.T. on orbit 2702. In both cases the measurements were made for a full moon. The field of vision of the telescope was 4' x 23', the average spectral resolution was 0.3μ and the time to record one spectrum was 4.5 s. Scanning was achieved by the orbital motion of Saljut 5; fig. 1 shows the region investigated. The place whence the sample of soil was taken from a depth of 2m is also marked. The thermal radiation spectrum of the Moon at >3μ was compared with that calculated from the temperature distribution along the region, assuming that the temperature of the sub-solar point is 395 K, and that the emissivity is unity everywhere. In such a way we have obtained the distribution of the emissivity e and that of the reflectivity R throughout the spectrum, assuming that R=1-e. A preliminary study of the reflectivity distribution along the whole length of the core sample was made between 1 and 2.2μ. To a depth of 130 cm, there is a region of relatively homogeneous regolith, with the reflectivity being close to its value for Mare samples. There is an increase of reflectivity between 130 cm and 220 cm which corresponds to a decrease of the secondary processed regolith and to the predominance of bedrock. Here there are narrow 3-5 cm thick layers where the reflectivity diminishes by a factor of 1.2 to 1.3. At the bottom of the core sample the mean value of reflectivity is 1.5 times larger than that of the top, approximating to values characteristic of the highland obtained from Luna 20. Samples from the depths of 118, 143 and 184 cm were chose for a more detail spectral study." @default.
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• W1530352014 date "1980-01-01" @default.
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• W1530352014 title "Infrared Reflection Spectra of the Moon and Lunar Soil" @default.
• W1530352014 doi "https://doi.org/10.1016/s0964-2749(13)60040-2" @default.
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