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

Liu, Tao; Li, Chaofeng; Ye, Lin

doi:10.1111/j.1945-5100.2011.01182.x

Cited by 14 publications

(10 citation statements)

References 28 publications

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“…The upper limit to the 4 He retention age is much lower than the Rb‐Sr age (177 ± 5 Ma) reported by Liu et al. () for GRV 99027 and the concordant Rb‐Sr and Sm‐Nd ages for other shergottites (~180 Ma) reported by Shih et al. (); however, this may be reasonable considering that this meteorite is heavily shocked and experienced slow cooling (Wang and Chen ).…”

Section: Cosmic Ray Exposure Historiesmentioning

confidence: 43%

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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: 43%

“…, ) contrast with “young” radiometric mineral isochrons, e.g., Sm‐Nd and Rb‐Sr (Liu et al. ). It is not yet understood whether this discrepancy is due to reset of the isochrons by alteration (Bouvier et al.…”

Section: Cosmic Ray Exposure Historiesmentioning

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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“…; Liu et al. ). It is possible that most lherzolitic shergottites came from the same igneous unit on Mars.…”

Section: Discussionmentioning

confidence: 98%

“…Most lherzolitic shergottites (including Y-793605, ALHA77005, LEW 88516, GRV 99027, Y-984028, NWA 1950, Y-000027/47/97) share similar bulk compositions, petrographies, and mineral chemistries (e.g., Lundberg et al 1990;Harvey et al 1993;Ebihara et al 1997;Ikeda 1997;Mikouchi and Miyamoto 1997;Warren and Kallemeyn 1997;Wadhwa et al 1999;Gillet et al 2005;Lin et al 2005;Hu et al 2011). In addition, they have ages close to approximately 180 Ma (Nyquist et al 2001;Borg et al 2002;Liu et al 2011). It is possible that most lherzolitic shergottites came from the same igneous unit on Mars.…”

Section: Genetic Link With Other Lherzolitic Shergottitesmentioning

confidence: 99%

Grove Mountains 020090 enriched lherzolitic shergottite: A two‐stage formation model

Miao

et al. 2013

Meteorit & Planetary Scien

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Abstract-Grove Mountains (GRV) 020090 is an enriched lherzolitic shergottite, distinct from other lherzolitic shergottites, except RBT 04262/1. Its characteristics include high abundance of plagioclase (24.2 vol% in the nonpoikilitic area), presence of K-feldspar, common occurrence of baddeleyite, high FeO contents of olivine (bimodal peaks at Fa 33 mol% and Fa 41 mol%) and low-Ca pyroxenes (bimodal peaks at Fs 23.8-31.7 mol% and Fs 25.7-33.9 mol%), and significant LREE enrichment of phosphates (500-610 9 CI). The bulk composition of GRV 020090 suggests derivation from partial melting of an enriched reservoir. However, the REE patterns of the cores of pigeonite oikocrysts and the olivine chadacrysts are indistinguishable from those of GRV 99027 and other moderately depleted lherzolitic shergottites, and reveal a LREE-depleted pattern of the primordial parent magma. We propose that the primordial parent magma of GRV 020090 was derived from a moderately depleted Martian upper mantle reservoir, and later the residual melt was contaminated by oxidized and enriched Martian crustal materials as it ascended up to the subsurface. GRV 020090 and RBT 04262/1 may have sampled an igneous unit different from other lherzolitic shergottites.

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“…Although so‐called “geochemically enriched” (i.e., only slightly depleted in LREE) shergottites and lherzolitic shergottites crystallized almost contemporaneously, their initial 87 Sr/ 86 Sr and ε 143Nd values differ significantly. The lherzolitic shergottites possess less radiogenic initial 87 Sr/ 86 Sr ratios of 0.7102–0.7105 and positive initial ε 143Nd values of ∼10 [ Shih et al , 1982; Morikawa et al , 2001; Borg et al , 2002; Misawa et al , 2006, 2008; Shih et al , 2011; Liu et al , 2011]. Thus, on the basis of REE patterns and isotopic systematics, RBT 04261 and RBT 04262 are classified into “geochemically enriched” shergottites like Shergotty, Zagami, and Los Angeles.…”

Section: Introductionmentioning

confidence: 99%

Uranium-lead age of baddeleyite in shergottite Roberts Massif 04261: Implications for magmatic activity on Mars

Niihara

2011

J. Geophys. Res.

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[1] The issue of the duration of Martian magmatic activity is one of the controversial debates recently: whether the young radiometric ages of $180 Ma for shergottites, a class of Martian meteorites, reflect the timing of crystallization from a magma or rather record later events related to shock metamorphism. In order to address the timescale over which Mars was geologically active, we have undertaken U-Pb isotopic studies on baddeleyite in the Roberts Massif (RBT) 04261 shergottite. Baddeleyite in RBT 04261 is usually associated with ilmenite and shows monoclinic structure, suggesting that the baddeleyite could have formed by crystallization from a residual liquid and not by shock metamorphism. In situ U-Th-Pb isotopic analyses of baddeleyite yield a young 238 U-206 Pb age of $200 Ma. Since the U-Pb system of baddeleyite is considered to be more resistant to resetting during reheating events, and olivine in RBT 04261 preserves an igneous calcium zoning, the young age of baddeleyite could be interpreted as a crystallization age of RBT 04261. The present results imply that Martian magma was still forming only 200 Ma ago, and that Mars had been geologically active until the recent past.

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

Cited by 14 publications

References 28 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

Grove Mountains 020090 enriched lherzolitic shergottite: A two‐stage formation model

Uranium-lead age of baddeleyite in shergottite Roberts Massif 04261: Implications for magmatic activity on Mars

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