High-resolution Earth-based lunar radar studies: Applications to lunar resource assessment

Details High-resolution Earth-based lunar radar studies: Applications to lunar resource assessment High-resolution Earth-based lunar radar studies: Applications to lunar resource assessment

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ntlr.work...48s&link_type=abstract

In Lunar and Planetary Inst., Joint Workshop on New Technologies for Lunar Resource Assessment p 48-49 (SEE N93-17233 05-91)

Astronomy and Astrophysics

Astronomy

Backscattering, Earth-Moon System, Lunar Surface, Radar Scattering, Radar Tracking, Regolith, Astronomical Observatories, High Resolution, Interferometry, Lunar Craters, Permittivity, Porosity, Spatial Resolution

Scientific paper

The lunar regolith will most likely be a primary raw material for lunar base construction and resource extraction. High-resolution radar observations of the Moon provide maps of radar backscatter that have intensity variations generally controlled by the local slope, material, and structural properties of the regolith. The properties that can be measured by the radar system include the dielectric constant, density, loss tangent, and wavelength scale roughness. The radar systems currently in operation at several astronomical observatories provide the ability to image the lunar surface at spatial resolutions approaching 30 m at 3.8 cm and 12.6 cm wavelengths and approximately 500 m at 70 cm wavelength. The radar signal penetrates the lunar regolith to a depth of 10-20 wavelengths so the measured backscatter contains contributions from the vacuum-regolith interface and from wavelength-scale heterogeneities in the electrical properties of the subsurface material. The three wavelengths, which are sensitive to different scale structures and scattering volumes, provide complementary information on the regolith properties. Aims of the previous and future observations include (1) analysis of the scattering properties associated with fresh impact craters, impact crater rays, and mantled deposits; (2) analysis of high-incidence-angle observations of the lunar mare to investigate measurement of the regolith dielectric constant and hence porosity; (3) investigation of interferometric techniques using two time-delayed observations of the same site, observations that require a difference in viewing geometry less than 0.05 deg and, hence, fortuitous alignment of the Earth-Moon system when visible from Arecibo Observatory.

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