Reconstruction of the Exposure Histories of 20 Allan Hills Ordinary Chondrites on the Basis of Cosmogenic 10Be, 26Al, Noble Gases, and Cosmic Ray Tracks

Details Reconstruction of the Exposure Histories of 20 Allan Hills Ordinary Chondrites on the Basis of Cosmogenic 10Be, 26Al, Noble Gases, and Cosmic Ray Tracks Reconstruction of the Exposure Histories of 20 Allan Hills Ordinary Chondrites on the Basis of Cosmogenic 10Be, 26Al, Noble Gases, and Cosmic Ray Tracks

Sep 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995metic..30s.556n&link_type=abstract

Meteoritics, vol. 30, no. 5, page 556

Other

Ages, Exposure, Terrestrial, Gases, Noble, Isotopes, Cosmogenic, Radionuclides

Scientific paper

Twenty ordinary chondrites from the 1988/89 meteorite search (ALH 88004, 88008, 88010, 88011, 88013, 88016 to 88021, 88026 to 88031, 88033, 88039, 88042) [1,2] were investigated for 10Be and 26Al, and for He, Ne and Ar by accelerator and rare gas mass spectrometry, respectively. Cosmic ray tracks were measured in samples of ALH 88019. Using theoretical production rates calculated by a physical model [3] the experimental data are interpreted with respect to the reconstruction of the preatmospheric exposure conditions and exposure histories of the meteoroids. Ordinary chondrites are particularly well suited to exemplify the capabilities of an interpretation of many cosmogenic nuclides measured in one sample. Model calculations of GCR production rates were performed for 10Be, 26Al, 3He, 21Ne, 22Ne and 38Ar as reported elsewhere [4,5]. For all meteorites, except for ALH 88019, the cosmogenic nuclide data can be explained by simple one stage exposure histories between 3 Ma and 44 Ma in meteoroids with radii between 5 cm and 85 cm. Exposure ages were derived from cosmogenic 3He, 21Ne and 38Ar on the basis of the theoretical production rates as function of3He/21Ne and 22Ne/21Ne as well as on the empirical ones proposed by Eugster [6]. The average ratios of exposure ages determined from theoretical production rates to those calculated according to Eugster [6] were 1.08+/-0.11, 1.11+/-0.25 and 1.12+/-0.17 in case of 3He, 21Ne and 38Ar, respectively. Repeated measurements of 10Be and 26Al in ALH 88019 resulted in 10.4+/-1.3 dpm/kg and 5.6+/-0.5 dpm/kg, respectively. But, the cosmogenic rare gas concentrations point to a (single stage) exposure age of 39 Ma in a meteoroid. This is in accordance with a measured cosmic ray track density in olivine of 2.8 * 10^6 cm^-2. The samples are from depths betwen 3 cm and 8 cm. Based on the track data we obtain a minimum meteoroid radius of 8 cm. The low 10Be and 26Al cannot be explained by a one stage exposure history and a long terrestrial age. Possible other exposure scenarios are discussed. Using the theoretical 10Be production rates and the 3He/21Ne and 22Ne/21Ne ratios, constraints about the sizes of the meteoroids and about the shielding depths in the samples were derived. 26Al was not used for this purpose since in four meteorites it is evidently affected by SCR production and since, generally, it could be changed due to long terrestrial residence times. However, most of the observed 26Al concentrations which are not affected by SCR production are consistent within experimental uncertainties with the expected GCR production rates. Substantial terrestrial age are proposed for ALH 88008, ALH 88029 and ALH 88030. Pairing among the investigated meteorites is discussed on the basis of rare gas data, 10Be and 26Al, and NTL data by Benoit et al. [7,8]. It can be concluded that the 20 meteorites result from at least 16 different falls. Acknowledgement: This work was supported by the Deutsche Forschungsgemeinschaft and the Swiss National Science Foundation. References: [1] Meteoritical Bulletin (1990) Meteoritics, 25, 237. [2] Meteoritical Bulletin (1991) Meteoritics, 26, 68. [3] Michel R. et al. (1991) Meteoritics, 26, 221-242. [4] Michel R. et al. (1995) Planet. Space Sci., in press. [5] Herpers U. et al. (1995) Planet. Space Sci., in press. [6] Eugster O. (1988) GCA, 52, 1649-1662. [7] Benoit P. H. et al. (1991) Meteoritics, 26, 262. [8] Benoit P. H. et al. (1992) Meteoritics, 27, 110.

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