Spectrogoniometric Measurements and Modeling of Apollo 16 Soil 68810

Details Spectrogoniometric Measurements and Modeling of Apollo 16 Soil 68810 Spectrogoniometric Measurements and Modeling of Apollo 16 Soil 68810

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p53a1498j&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #P53A-1498

Other

[5464] Planetary Sciences: Solid Surface Planets / Remote Sensing, [6250] Planetary Sciences: Solar System Objects / Moon

Scientific paper

Laboratory visible/near-infrared multispectral goniometer observations of Apollo 16 mature highland soil 68810,2 were acquired using the Bloomsburg University Goniometer (BUG) [1]. These data provided constraints on Hapke radiative transfer models for comparison to model results from similar BUG data acquired of Apollo 11 soil 10084 [2]. Such data are relevant to analyses of lunar surface observations acquired by orbital cameras and spectrometers flown on past and present lunar missions. Standard BUG measurements were acquired (incidence 0-60°, emission 0-80°, and phase 3-140°) comprising 680 measurements per wavelength. We acquired multispectral measurements of the 68810 sample at 450, 550 ,700, 750, 850, and 950 nm. We also supplemented this geometric coverage by constructing an elongated sample holder for measurements in and perpendicular to the principal plane. These measurements were acquired at 450, 550, 750, and 950 nm, and allowed expanded geometric coverage to incidence angles of 0-75° and phase angles of 3-155°, comprising 765 measurements per wavelength. Hapke radiative transfer models were run using 1-term and 2-term Henyey-Greenstein (HG) phase functions to determine photometric properties such as single scattering albedo and backscattering behavior. The results show little difference in the photometric parameters between model runs using the standard and expanded data sets. Models of the 68810 highland sample exhibit higher single scattering albedo (by ~66%) than the 10084 mare sample models, consistent with modeling of Clementine and other remote sensing observations [e.g., 3]. The 68810 soil is also slightly more broadly backscattering (in both 1-term and 2-term HG models), with properties similar to results from laboratory analyses of agglutinates and rough, clear spheres. Both Apollo soils are more backscattering than any lunar analog soil yet measured [2]. The opposition effect width h (compaction parameter) is slightly smaller for the 68810 highland soil (h=0.031), suggesting a less uniform average grain size and/or more porous soil than the 10084 mare soil (h=0.040). This is consistent with the comparison of highland and mare regions from [4]. [1] Foote, E., et al., this volume; [2] Johnson, J.R., et al., Spectrogoniometric Measurements and Modeling of Apollo 11 Soil 10084, Lunar Plan. Sci. Conf. XL, # 1427, 2009; [3] Hillier, J. et al., Multispectral photometry of the Moon and absolute calibration of the Clementine UV/Vis camera, Icarus, 141, 205-225, 1999; [4] Helfenstein, P., and Veverka, J., Photometric properties of lunar terrains derived from Hapke’s equation, Icarus, 72, 342-357, 1987.

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