Comment on “Update on terrestrial ages of Antarctic meteorites” by K. Nishiizumi, D. Elmore and P.W. Kubik

Sears, D. W. G.; Hasan, F. A.; Myers, Benjamin; Sears, H.

doi:10.1016/0012-821x(90)90141-j

Cited by 5 publications

(2 citation statements)

References 11 publications

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“…Nineteen of the samples plot on a trend in which natural TL decreases by a factor of 100, while 26 Al decreases by a factor of 6. This is consistent with a number of detailed studies over many years that suggested that natural TL, like 26 Al, could be used to estimate terrestrial ages (Sears and Mills 1974;Sears and Durrani 1980;Melcher 1981a;Sears et al 1990).…”

Section: Introductionsupporting

confidence: 90%

The natural thermoluminescence of Antarctic meteorites and their terrestrial ages and orbits: A 2010 update

Sears

Yozzo

Ragland

2011

Meteorit & Planetary Scien

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Abstract-We have examined the relationship between natural thermoluminescence (TL) and 26 Al in 120 Antarctic meteorites in order to explore the orbital history and terrestrial ages of these meteorites. Our results confirm the observations of Hasan et al. (1987) which were based on 23 meteorites. For most meteorites there was a positive correlation between natural TL and 26 Al, reflecting their similarity in decay rate under Antarctic conditions and thus in terrestrial age. For a small group with low TL and high 26 Al a small perihelion was proposed. Within this group, natural TL decreases with terrestrial age as determined by 36 Cl measurements, although the rate of TL decay is faster (half-life approximately 10 ka) and the ages that can be determined are smaller (<200 ka) than for most meteorites. The faster decay rate and lower natural TL levels are a reflection of recent exposure to higher radiation doses and higher temperatures, since this history would populate less stable TL traps with smaller electron densities. We sort the 120 meteorites by perihelion and terrestrial age. The normal perihelion group range up to approximately 1000 ka and the small perihelion group range up to approximately 200 ka. An intermediate perihelion group tends to have short terrestrial ages (20-60 ka). There is acceptable agreement between most (34 out of 43) of our present terrestrial age estimates and those determined by isotopic means, the exceptions reflecting complex irradiation histories, long burial times in the Antarctic, or other issues.

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Section: Introductionsupporting

confidence: 90%

The natural thermoluminescence of Antarctic meteorites and their terrestrial ages and orbits: A 2010 update

Sears

Yozzo

Ragland

2011

Meteorit & Planetary Scien

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“…Other major constituents include AOIs, CAIs, Fe-Ni metal, and lithic fragments that are typically isolated olivine crystals (McSween 1977a(McSween , 1977bRubin et al 1985). As reviewed in Cloutis et al (2012d), several authors have further subdivided the CO chondrites based on metamorphic properties (e.g., McSween 1977b;Scott & Jones 1990;Sears et al 1991;Chizmadia et al 2002;Greenwood & Franchi 2004). Like main petrologic types, petrologic subtypes are numbered to correspond with increasing metamorphic processing, with known CO samples ranging from 3.1 to 3.8 (Meteoritical Bulletin Database).…”

Section: Kainsaz (Co32)mentioning

confidence: 99%

Grain Size Effects on UV–MIR (0.2–14 μm) Spectra of Carbonaceous Chondrite Groups

Cantillo,

Reddy,

Battle

et al. 2023

Planet. Sci. J.

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Carbonaceous chondrites are among the most important meteorite types and have played a vital role in deciphering the origin and evolution of our solar system. They have been linked to low-albedo C-type asteroids, but due to subdued absorption bands, definitive asteroid–meteorite linkages remain elusive. A majority of these existing linkages rely on fine-grained (typically < 45 μm) powders across a limited wavelength range in the visible to near-infrared (0.35–2.5 μm). While this is useful in interpreting the fine-grained regolith of larger main-belt objects like Ceres, recent spacecraft missions to smaller near-Earth asteroids (NEAs), such as Bennu and Ryugu, have shown that their surfaces are dominated by larger grain size material. To better interpret the surfaces of these smaller, carbonaceous NEAs, we obtained laboratory reflectance spectra of seven carbonaceous chondrite meteorite groups (CI, CM, CO, CV, CR, CK, C2-ungrouped) over the ultraviolet to mid-infrared range (0.2–14 μm). Each meteorite contained five grain size bins (45–1000 μm) to help constrain spectral grain size effects. We find a correlation between grain size and absolute reflectance, spectral slope, band depth, and the Christiansen feature band center. Principal component analysis of grain size variation illustrates a similar trend to lunar-style space weathering. We also show that the Bus–DeMeo asteroid taxonomic classification of our samples is affected by grain size, specifically shifting CM2 Aguas Zarcas from a Ch-type to B-type with increasing grain size. This has implications for the parent body of the OSIRIS-REx target, Bennu. With Aguas Zarcas, we present results from Hapke modeling.

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Study of terrestrial ages of the Antarctic meteorites with thermoluminescence

Miono

Nakanishi

1993

Il Nuovo Cimento C

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Comment on “Update on terrestrial ages of Antarctic meteorites” by K. Nishiizumi, D. Elmore and P.W. Kubik

Cited by 5 publications

References 11 publications

The natural thermoluminescence of Antarctic meteorites and their terrestrial ages and orbits: A 2010 update

The natural thermoluminescence of Antarctic meteorites and their terrestrial ages and orbits: A 2010 update

Grain Size Effects on UV–MIR (0.2–14 μm) Spectra of Carbonaceous Chondrite Groups

Study of terrestrial ages of the Antarctic meteorites with thermoluminescence

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