Albedo measurements on meteorite particles fn1 fn1Presented at ACM96, Versailles, 8–12.7.1996. Also University of Pisa, Department of Mathematics, Pisa, Italy.

Piironen, J.; Muinonen, K.; Nousiainen, Timo; Sasse, Christian; Roth, S.; Peltoniemi, Jouni

doi:10.1016/s0032-0633(98)00035-x

Cited by 17 publications

(6 citation statements)

References 7 publications

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“…The NEATM albedo values for these classes are lower in value than the STM derived albedos. The NEATM albedo range best-matches the spectroscopically inferred compositions of S-and C-class asteroids as suggested by laboratory albedo measurements of ordinary chondrite and carbonaceous chondrite materials (Piironen et al 1998 into the near-IR, could provide a basic taxonomic classification of a newly discovered object reliable enough to obtain an asteroid diameter within ∼ 10%. However, the veracity of this assertion cannot be assessed as asteroids selected for our thermal analysis (Table 1) are sufficiently large enough in size that they would have saturated the SDSS images and are thus not present in their moving target catalog (Ivezić et al 2002).…”

Section: Sparse-sampling Effectssupporting

confidence: 64%

RECTIFIED ASTEROID ALBEDOS AND DIAMETERS FROMIRASANDMSXPHOTOMETRY CATALOGS

Ryan¹,

Woodward²

2010

The Astronomical Journal

116

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Rectified diameters and albedo estimates of 1517 main belt asteroid selected from the IRAS and MSX asteroid photometry catalogues are derived from updated infrared thermal models, the Standard Thermal Model (STM) and the Near Earth Asteroid Thermal Model (NEATM), and Monte Carlo simulations, using new Minor Planet Center (MPC) compilations of absolute magnitudes (Hvalues) constrained by occultation and radar derived parameters. The NEATM approach produces a more robust estimate of albedos and diameters, yielding albedos of p v (NEATM mean)= 0.081 ± 0.064. The asteroid beaming parameter (η) for the selected asteroids has a mean value of 1.07 ± 0.27, and the smooth distribution of η suggests that this parameter is independent of asteroid properties such as composition. No trends in η due to size-dependent rotation rates are evident. Comparison of derived η's as a function of taxonomic type indicates the beaming parameter values for S-type and C-type asteroids are identical within the standard deviation of the population of beaming parameters.

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Section: Sparse-sampling Effectssupporting

confidence: 64%

RECTIFIED ASTEROID ALBEDOS AND DIAMETERS FROMIRASANDMSXPHOTOMETRY CATALOGS

Ryan¹,

Woodward²

2010

The Astronomical Journal

116

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“…(3)) be p < 0.2 and that the volume-element single-scattering albedos beω V > 0.5. Such single-scattering albedos are comparable to the corresponding albedos measured in the laboratory for single lunar analog particles large compared to the wavelength (Piironen et al 1998). The geometric-albedo range for the mare regions has been estimated with the help of the study by Lumme & Irvine (1982).…”

Section: Scattering Model For Mare Regionssupporting

confidence: 66%

Lunar mare single-scattering, porosity, and surface-roughness properties with SMART-1 AMIE

Muinonen

Parviainen

Näränen

et al. 2011

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A novel shadowing and coherent-backscattering model is utilized in the analysis of the single-scattering albedos and phase functions, local surface roughness, and regolith porosity of specific lunar mare regions imaged by the AMIE camera (Advanced Moon micro-Imager Experiment) onboard ESA SMART-1 mission. Shadowing due to the regolith particles is accounted via ray-tracing computations for densely-packed particulate media with a fractional-Brownian-motion interface with free space. The shadowing modeling allows us to derive the scattering phase function for a ∼100-μm volume element of the lunar mare regolith. The volume-element phase function is explained by coherent-backscattering modeling, where the fundamental single scatterers are the wavelength-scale particle inhomogeneities or the smallest fraction of the particles on the lunar surface. The phase function of the fundamental scatterers is expressed as a sum of two Henyey-Greenstein terms, accounting for increased backward scattering as well as increased forward scattering. Based on the modeling of the AMIE lunar photometry, we conclude that most of the lunar mare opposition effect is caused by coherent backscattering within volume elements comparable in size to typical lunar particles, with only a small contribution from shadowing effects.

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“…Piironen et al (1998) determined the single particle albedos of ordinary chondrites and C2 carbonaceous chondrites to be 0.50 ± 0.25 and 0.15 ± 0.02, respectively. Use of the Lumme-Bowell scattering model (Lumme & Bowell 1981) with these values yields geometric albedos of 0.13-0.24 for ordinary chondrites and 0.04-0.07 for carbonaceous chondrites.…”

Section: Comparisons To Previous Resultsmentioning

confidence: 99%

ExploreNEOs. V. AVERAGE ALBEDO BY TAXONOMIC COMPLEX IN THE NEAR-EARTH ASTEROID POPULATION

Thomas

Trilling

Emery

et al. 2011

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Examining the albedo distribution of the near-Earth object (NEO) population allows for a better understanding of the relationship between absolute (H) magnitude and size, which impacts calculations of the size frequency distribution and impact hazards. Examining NEO albedos also sheds light on the differences between the NEO and Main Belt populations. We combine albedo results from the ExploreNEOs Warm Spitzer Exploration Science program with taxonomic classifications from the literature, publicly available data sets, and new observations from our concurrent spectral survey to derive the average albedos for C-, D-, Q-, S-, V-, and X-complex NEOs. Using a sample size of 118 NEOs, we calculate average albedos of 0.29 −0.01 , but these averages are based on a small number of objects (five and two, respectively) and will improve with additional observations. We use albedos to assign X-complex asteroids to one of the E-, M-, or P-types. Our results demonstrate that the average albedos for the C-, S-, V-, and X-complexes are higher for NEOs than the corresponding averages observed in the Main Belt.

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Albedo measurements on meteorite particles fn1 fn1Presented at ACM96, Versailles, 8–12.7.1996. Also University of Pisa, Department of Mathematics, Pisa, Italy.

Cited by 17 publications

References 7 publications

RECTIFIED ASTEROID ALBEDOS AND DIAMETERS FROMIRASANDMSXPHOTOMETRY CATALOGS

RECTIFIED ASTEROID ALBEDOS AND DIAMETERS FROMIRASANDMSXPHOTOMETRY CATALOGS

Lunar mare single-scattering, porosity, and surface-roughness properties with SMART-1 AMIE

ExploreNEOs. V. AVERAGE ALBEDO BY TAXONOMIC COMPLEX IN THE NEAR-EARTH ASTEROID POPULATION

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