Mapping of regolith layer thickness for the lunar nearside is carried out with Arecibo radar data at 70 cm wavelength (T. W. Thompson 1987, Earth Moon Planets 37, 59-70) and distributions of iron and titanium content derived from Earth-based optical data (Yu. Shkuratov et al. 1999, Icarus 137, 222-2
Radar mapping of the Moon
β Scribed by Hughes, David W.
- Book ID
- 109692221
- Publisher
- Nature Publishing Group
- Year
- 1974
- Tongue
- English
- Weight
- 233 KB
- Volume
- 250
- Category
- Article
- ISSN
- 0028-0836
- DOI
- 10.1038/250375a0
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We are grateful to Dr. B. Campbell for his comment, as this gives an opportunity to discuss once again important problems concerning radar studies of the lunar surface and to compare the two model approaches presented in (Campbell et al. 1997) and our paper (Shkuratov and Bondarenko 2001). Before w
In a recent Icarus article, Shkuratov and Bondarenko (2001) propose a model for the depth of the lunar regolith based on 70-cm radar observations and near-infrared spectroscopy. This model treats the regolith as a single homogeneous layer of lossy dust, and ignores scattering by buried rocks. There