Focused 70-cm Wavelength Radar Mapping of the Moon

Campbell, B. A.; Campbell, D. B.; Margot, Jean-Luc; Ghent, R. R.; Nolan, M. C.; Chandler, J. F.; Carter, L.M.; Stacy, N.J.S.

doi:10.1109/tgrs.2007.906582

Cited by 89 publications

(98 citation statements)

References 25 publications

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“…Thus, radar images of the Moon appear similar to visual photographs of sunlit terrain. Figure 6 shows the scattering differences from slopes and diffuse scattering enhancements in the 70 cm radar images [Campbell et al, 2007] [15] An empirical model is developed in Appendix A for radar scattering differences associated with rough surfaces of young lunar craters, thin regolith over ice, and ice patches occupying part of the radar pixel. The key assumption is that radar scattering from the lunar surface is the sum of specular and diffuse scattering components, as shown in Figures 2 and 7.…”

Section: Overview Of Lunar Radar Scatteringmentioning

confidence: 99%

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Modeling radar scattering from icy lunar regoliths at 13 cm and 4 cm wavelengths

Thompson¹,

Ustinov²,

Heggy³

2011

J. Geophys. Res.

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[1] Two orbital synthetic aperture radars (SARs), the Chandrayaan-1 Mini-SAR (13 cm wavelength) and the Lunar Reconnaissance Orbiter (LRO) Mini-RF (13 and 4.2 cm wavelengths), have been imaging the lunar surface searching for ice deposits in the polar permanently shadowed areas. To understand the radar signatures of lunar polar ices, an empirical two-component model with parametric variations of the specular and diffuse components was developed and validated. This model estimates scattering differences associated with slopes, surface roughness, thin regolith over ice, and patches of ice. Lunar radar backscatter cross sections for the average surface for the Chandrayaan-1 and LRO instruments are estimated from the radar cross sections from the Moon at 3.8, 23, and 68 cm wavelengths measured in the 1960s at the Massachusetts Institute of Technology. This modeling predicts that enhanced diffuse scattering from near-surface ice can be separated from rocks if the scattering is characterized by both the high reflectivity and circular polarization ratios (CPRs) like those observed on Mercury, Mars, and the Galilean satellites. Scattering from near-surface ices covered by a thin regolith can be separated from rocks if the enhancement is twice the average or more. If, however, the lunar ice is dispersed throughout the regolith as ice-filling pores, then scattering differences might be too small to detect. Preliminary validation using LRO radar data for a few polar and midlatitude craters indicate that the observed CPRs are consistent with our models for different regolith ice and roughness conditions. Citation: Thompson, T. W., E. A. Ustinov, and E. Heggy (2011), Modeling radar scattering from icy lunar regoliths at 13 cm and 4 cm wavelengths,

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Section: Overview Of Lunar Radar Scatteringmentioning

confidence: 99%

“…Maurolycus is an even older, Nectarian-aged crater, where echo modulations across the crater result only from slope modulation of the radar echoes. Radar data are from Campbell et al [2007]; pixel size is 400-500 m. North is at the top.…”

Section: Overview Of Lunar Radar Scatteringmentioning

confidence: 99%

Modeling radar scattering from icy lunar regoliths at 13 cm and 4 cm wavelengths

Thompson¹,

Ustinov²,

Heggy³

2011

J. Geophys. Res.

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“…3) wavelengths, using the Arecibo and Green Bank telescopes. The images are obtained by transmitting a circularly polarized signal and receiving both reflected circular polarization states (Campbell et al, 2007). Reflections that match the polarization expected from a mirror-like siuface are termed opposite-sense circular (OC), and those with the orthogonal polarization state are termed same-sense circular (SC).…”

Section: Remote Sensing Datamentioning

confidence: 99%

Volcanic and impact deposits of the Moon's Aristarchus Plateau: A new view from Earth-based radar images

Campbell¹,

Carter²,

Hawke³

et al. 2008

Geol

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Lunar pyroclastic deposits reflect an explosive stage of tlie basaltic volcanism that filled impact basins across the nearside. These fine-grained mantUng layers are of interest for their association with early mare volcanic processes, and as possible sources of volatiles and other species for lunar outposts. We present Earth-based radar images, at 12.6 and 70 cm wavelengths, of the pyroclastic deposit that blankets the Aristarchus Plateau. The 70 cm data reveal the outlines of a lava-flow complex that covers a signiflcant portion of the plateau and appears to have formed by spillover of magma from the large sinuous rille Vallis Schröteri. The pyroclastics mantling these flows are heavily contaminated with rocks 10 cm and larger in diameter. The 12.6 cm data confirm that other areas are mantled by 20 m or less of material, and that there are numerous patches of 2 cm and larger rocks associated with éjecta from Aristarchus crater. Some of the radar-detected rocky debris is within the mantling material and is not evident in visible-wavelength images. The radar data identify thick, rock-poor areas of the pyroclastic deposit best suited for resource exploitation.

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“…Complementary information on the physical properties of the upper 10 m or more of the regolith may be obtained from imaging radar observations, but until recently (Campbell et al, 2007a(Campbell et al, , 2007b) the coverage and resolution of such data have not been sufficient for detailed investigations of areas near the lunar limb. With the new observations presented here, we can examine the influence of Orientale éjecta on the southern highlands megaregolith.…”

Section: Introductionmentioning

confidence: 99%

Earth-based radar data reveal extended deposits of the Moon's Orientale basin

Ghent

Campbell

Hawke

et al. 2008

Geol

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We present new Earth-based radar observations of éjecta associated with the lunar Orientale impact basin. We can distinguish (1) a block-poor éjecta fades composing a concentric halo of mantling material 10 m or greater in thickness that extends more than 1000 km from the basin center, and (2) a melt-rich deposit that forms a discontinuous but areally extensive stratigraphie marker across the southern highlands. The melt-rich component likely extends well into the South Pole-Aitken basin, a key target for future landed and sample return missions. The observation of these two éjecta fades and their distribution across the southern nearside yields new insight into the types and distribution of material contributed by large basin-forming impacts to the highlands megaregoUth.

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Focused 70-cm Wavelength Radar Mapping of the Moon

Cited by 89 publications

References 25 publications

Modeling radar scattering from icy lunar regoliths at 13 cm and 4 cm wavelengths

Modeling radar scattering from icy lunar regoliths at 13 cm and 4 cm wavelengths

Volcanic and impact deposits of the Moon's Aristarchus Plateau: A new view from Earth-based radar images

Earth-based radar data reveal extended deposits of the Moon's Orientale basin

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