Lunar surface mechanical properties-Surveyor 1

Christensen, E. M.; Batterson, S. A.; Benson, H. E.; Chandler, C. E.; Jones, Rebecca H.; Scott, Ronald F.; Shipley, E. N.; Sperling, F. B.; Sutton, George H.

doi:10.1029/jz072i002p00801

Cited by 38 publications

(11 citation statements)

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“…From our estimation, the estimated filling factor for MI 62231SaS ranges from 0.13 to 0.26 (and thus from 0.4 to 0.8 in bulk density). These values are lower than the previously estimated filling factor of 0.5, which corresponds to a bulk density of 1.3 to 1.6, for the top 15 cm surface of the regolith (Duke et al 1970;Christensen et al 1967;Mitchell et al 1974). This may suggest the possibility that the topmost layer of the surface (possibly a few millimeters) of the lunar regolith is more porous than the deeper layers.…”

Section: Derivation Of MI Correction Coefficientcontrasting

confidence: 47%

Deriving the Absolute Reflectance of Lunar Surface Using SELENE (Kaguya) Multiband Imager Data

et al. 2010

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The absolute reflectance of the Moon has long been debated because it has been suggested (Hillier et al. in Icarus 151:205-225, 1999) that there is a large discrepancy be-M. Ohtake ( ) · T. Morota · J. Haruyama · H. Otake 58 M. Ohtake et al.tween the absolute reflectance of the Moon derived from Earth-based telescopic data and that derived from remote-sensing data which are calibrated using laboratory-measured reflectance spectra of Apollo 16 bulk soil 62231. Here we derive the absolute reflectance of the lunar surface using spectral data newly acquired by SELENE (Kaguya) Multiband Imager and Spectral Profiler. The results indicate that the reflectance of the Apollo 16 standard site, which has been widely used as an optical standard in previous Earth-based telescopic and remote-sensing observations derived by Multiband Imager, is 47% at 415 nm and 67% to 76% at 750 to 1550 nm of the value for the Apollo 16 mature soil measured in an Earth-based laboratory. The data also suggest that roughly 60% of the difference is caused by the difference in soil composition and/or maturity between the 62231 sampling site and the Apollo 16 standard site and that the remaining 40% difference can be explained by the difference between the compaction states of the laboratory and the actual lunar surface. Consideration of the compaction states of the surface soil demonstrates its importance for understanding the spectral characteristics of the lunar surface. We also explain and evaluate data analysis procedures to derive reflectance from Multiband Imager data.Keywords Moon · Kaguya · SELENE · Multiband Imager · Reflectance Abbreviations A16StSApollo 16 standard site used by Clementine UVVIS camera as an optical standard site; located about 10 km west of the Apollo 16 landing site. MI or SP or ROLO data of A16StS is denoted as MI or SP or ROLO A16StS. The number after A16StS indicates the observation number for MI and SP corrected RLab62231 RLab62231 corrected using the correction factors in Hillier et al. (1999) Diff lab-MI Difference of reflectance spectra between RLab62231 and MI A16StS Diff lab-EbtDifference of reflectance spectra between RLab62231 and Earth-based telescopic data in Shorthill et al. (1969)

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Section: Derivation Of MI Correction Coefficientcontrasting

confidence: 47%

Deriving the Absolute Reflectance of Lunar Surface Using SELENE (Kaguya) Multiband Imager Data

et al. 2010

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“…Prior to the Apollo missions, a very low bulk density of 0.3–0.4 g/cm

^{3}

for the lunar surface was inferred through remote sensing observations (Halajian, ; Jaffe, ). Subsequent in situ robotic measurements at the Surveyor and Luna landing sites indicated an average surficial bulk density of about 1.5 g/cm

^{3}

(Christensen et al, ; Leonovich et al, ; Scott & Roberson, ). In situ bulk density analysis of the lunar regolith was also deduced from analyses of astronaut bootprint, vehicle track, boulder track, and penetration resistance, with values varying from 1.3 to 1.7 g/cm

^{3}

and an upper limit between 1.81 and 1.92 g/cm

^{3}

(Mitchell et al, ).…”

Section: Introductionmentioning

confidence: 99%

Bulk Density of the Lunar Regolith at the Chang'E‐3 Landing Site as Estimated From Lunar Penetrating Radar

2020

Earth and Space Science

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Bulk density of the lunar regolith is a key factor affecting its geophysical and geotechnical properties. In this study, a new method for estimating the bulk density of the lunar regolith is developed based on the geometric characteristic (i.e., hyperbolic shape) of radar echoes in ground penetrating radar (GPR) image. As an application, bulk density of the lunar regolith at China's Chang'E‐3 (CE‐3) landing site is estimated using the Lunar Penetrating Radar data. In total, 57 hyperbolas are identified in the Lunar Penetrating Radar image and their eccentricities are used to estimate relative permittivity of the regolith. Then, bulk density of the lunar regolith is estimated using an empirical relation through its dependence on relative permittivity. The results show that bulk density of the regolith at the CE‐3 landing site increases with depth from 0.85 g/cm 3 at the surface to a steady‐state value of 2.25 g/cm 3 at 5 m, with an average gradient much smaller than that based on the Apollo regolith samples. The bulk density corresponds to a regolith porosity of 74.5% at the surface and 32.3% at 5 m depth over the CE‐3 landing region. Given that the landing site is only ∼50 m from the east rim of a 500 m diameter crater, named as Zi Wei, the steady‐state bulk density indicates a 29% volume fraction of subsurface rocks within the continuous ejecta of this crater.

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“…Christensen et al [1967]). An approximate analysis of the unstroked Surveyor landing gear elasticity indicates that the first vertical translatory spacecraft mode has a frequency of 8.0 Hz ----_10% for the spacecraft supported by its landing legs on a rigid surface.…”

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Lunar surface mechanical properties at the landing site of Surveyor 3

Christensen¹,

Batterson²,

Benson³

et al. 1968

J. Geophys. Res.

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Analyses of engineering and television data returned by Surveyor 3 indicate that the mechanical properties of the lunar surface material inside the crater in which the spacecraft landed are similar to the mechanical properties of the level mare area at the Surveyor 1 landing site. The static bearing strength ranges from 2 to 6 newtons/cm2 for a penetration depth between 2 and 5 cm and a bearing diameter between 20 and 30 cm. The soil cohesion is less than 1 newton/cm2; its rigidity modulus is low. A substantial percentage of the particles of the lunar surface material appear to be smaller than 0.06 mm in diameter, and a significant number are under 0.01 mm. The fine structure of the surface can be deformed substantially by applying a small, distributed, compressive force.

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Lunar surface mechanical properties-Surveyor 1

Cited by 38 publications

References 0 publications

Deriving the Absolute Reflectance of Lunar Surface Using SELENE (Kaguya) Multiband Imager Data

Deriving the Absolute Reflectance of Lunar Surface Using SELENE (Kaguya) Multiband Imager Data

Bulk Density of the Lunar Regolith at the Chang'E‐3 Landing Site as Estimated From Lunar Penetrating Radar

Lunar surface mechanical properties at the landing site of Surveyor 3

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