Cosmic-ray exposure age of Martian meteorite GRV 99027

Kong, Ping; Fabel, Derek; Brown, Robert D.; Freeman, Stewart P.H.T.

doi:10.1007/s11430-007-0089-6

Cited by 8 publications

(20 citation statements)

References 18 publications

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“…Our adopted noble gas CRE age for GRV 99027 is ~29% greater than the 4.4 ± 0.6 Ma CRE age determined by Kong et al. () based on 10 Be data and a now‐obsolete 10 Be half‐life of 1.51 Ma. We expect that this discrepancy is most likely due to differing estimates of shielding depth, and therefore, of the 10 Be saturation activity.…”

Section: Cosmic Ray Exposure Historiesmentioning

confidence: 52%

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The noble gas concentrations of the Martian meteorites GRV 99027 and paired NWA 7906/NWA 7907

Stephenson

Lin

Leya

2017

Meteorit & Planetary Scien

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Here we present the isotopic concentrations of He, Ne, Ar, Kr, and Xe for the three Martian meteorites, namely Grove Mountains 99027 (GRV 99027), Northwest Africa 7906 (NWA 7906), and Northwest Africa 7907 (NWA 7907). The cosmic ray exposure (CRE) age for GRV 99027 of 5.7 ± 0.4 Ma (1σ) is consistent with CRE ages for other poikilitic basaltic shergottites and suggests that all were ejected in a single event ~5.6 Ma ago. After correcting for an estimated variable sodium concentration, the CRE ages for NWA 7906 and NWA 7907 of 5.4 ± 0.4 and 4.9 ± 0.4 Ma (1σ), respectively, are in good agreement with the CRE age of ~5 Ma favored by Cartwright et al. () for NWA 7034. The data, therefore, support the conclusion that all three basaltic regolith breccias are paired. The 40Ar gas retention age for NWA 7907 of ~1.3 Ga is in accord with Cartwright et al. (). For NWA 7906, we were unable to determine a 40Ar gas retention age. The 4He gas retention ages for NWA 7906 and 7907 are in the range of 200 Ma and are much shorter than the 40Ar gas retention age of NWA 7907, indicating that about 86–88% of the radiogenic 4He has been lost. The Kr and Xe isotopic concentrations in GRV 99027 are composed almost exclusively of Martian interior (MI) gases, while for NWA 7906 and NWA 7907, they indicate gases from the MI, elementally fractionated air, and possibly Martian atmosphere.

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Section: Cosmic Ray Exposure Historiesmentioning

confidence: 52%

“…) GRV 99027 has been previously studied for 10 Be and 26 Al (Kong et al. ) but not for noble gases. NWA 7906 and NWA 7907 are both likely pairs of NWA 7034 (Ruzicka et al.…”

Section: Introductionmentioning

confidence: 99%

The noble gas concentrations of the Martian meteorites GRV 99027 and paired NWA 7906/NWA 7907

Stephenson

Lin

Leya

2017

Meteorit & Planetary Scien

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“…This suggests that GRV 99027 may have been ejected from the same igneous unit on Mars as the others, by a single impact event (Lin et al. 2005, 2008b; Kong et al. 2007).…”

Section: Introductionmentioning

confidence: 96%

“…2004; Lin et al. 2005, 2008b), and has the same ejection age of approximately 4 Ma (Kong et al. 2007).…”

Section: Introductionmentioning

confidence: 99%

Rb‐Sr and Sm‐Nd isotopic systematics of the lherzolitic shergottite GRV 99027

Liu

2011

Meteorit & Planetary Scien

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Abstract-Rb-Sr and Sm-Nd isotopic analyses of the lherzolitic shergottite Grove Mountains (GRV) 99027 are reported. GRV 99027 yields a Rb-Sr mineral isochron age of 177 ± 5 (2r) Ma and an initial 87 Sr ⁄ 86 Sr ratio (I Sr ) of 0.710364 ± 11 (2r). Due to larger uncertainties of the Sm-Nd isotopic data, no Sm-Nd isochron age was obtained for GRV 99027. The e 143 Nd value is estimated approximately +12.2, assuming an age of 177 Ma. The I Sr of GRV 99027 is distinguishable from other lherzolitic shergottites, confirming our previous conclusion that it is not paired with them (Lin et al. 2005). The new data of GRV 99027 support the same age of approximately 180 Ma for most lherzolitic shergottites, and fill the small gap of I Sr between Allan Hills A77005 and Lewis Cliff 88516 (Borg et al. 2002). All available data are consistent with a single igneous source for the intermediate subgroup of lherzolitic shergottites.

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“…An intensive study of the first three lherzolitic shergottites (i. isochron ages [7,8] and ejection events [9][10][11] among them. Thus, lherzolitic shergottites could have been ejected from the same igneous unit on Mars by a single impact event.…”

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confidence: 99%

Petrography, mineral chemistry and shock metamorphism of Yamato 984028 lherzolitic shergottite

Feng

2011

Chin. Sci. Bull.

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Y984028 is a new lherzolitic shergottite, consisting of poikilitic and non-poikilitic lithologies. The mafic silicates are FeO-poor, and the chromite is TiO 2 -poor in the poikilitic lithology compared to the grains in the non-poikilitic lithology. This meteorite shares similar mineral petrography and mineral chemistry with GRV 99027, but is not paired with the latter because of their different shock-induced features. Y984028 was severely shocked and experienced no significant thermal metamorphism after the main impact event. Hence, Y984028 serves as a probe for the study of meteorite impact processes on terrestrial surfaces. The melt veins in Y984028 are characterized by the absence of any high-pressure polymorphs, the presence of abundant small mineral fragments, and the prevailing granulation textures of olivine and chromite. These features are consistent with adiabatic melting during the release of shock-induced high-pressure and quenching at ambient pressure. [19,20]), are significantly evolved with high abundances of rare Earth elements (REEs) and other incompatible elements. Study of new samples is clearly important for identifying the petrogenesis of lherzolitic shergottites. Mars

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Cosmic-ray exposure age of Martian meteorite GRV 99027

Cited by 8 publications

References 18 publications

The noble gas concentrations of the Martian meteorites GRV 99027 and paired NWA 7906/NWA 7907

The noble gas concentrations of the Martian meteorites GRV 99027 and paired NWA 7906/NWA 7907

Rb‐Sr and Sm‐Nd isotopic systematics of the lherzolitic shergottite GRV 99027

Petrography, mineral chemistry and shock metamorphism of Yamato 984028 lherzolitic shergottite

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