Sayh al Uhaymir 094: A new martian meteorite from the Oman desert

Gnos, Edwin; Hofmann, Beda A.; Franchi, I. A.; Al-Kathiri, A.; Huser, M.; Moser, Linda

doi:10.1111/j.1945-5100.2002.tb00859.x

Cited by 53 publications

(78 citation statements)

References 33 publications

(24 reference statements)

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“…1) and have been described as olivine-phyric shergottites or picritic shergottites (Gnos et al 2002;Goodrich 2003). This includes lithology A of EETA79001.…”

Section: Olivine-rich Shergottitesmentioning

confidence: 99%

The SNC meteorites: basaltic igneous processes on Mars

Bridges

Warren²

2006

JGS

135

128

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A group of 32 meteorites, the SNC (Shergotty, Nakhla, Chassigny) group, was derived from Mars as a product of 4-7 ejection events, probably from Tharsis and Elysium-Amazonis. The SNCs either have basaltic mineralogy or some are ultramafic cumulates crystallized from basaltic melts. The SNCs can be classified both petrographically and geochemically. We classify the shergottite SNC meteorites on the basis of their light rare earth element (LREE) depletion into highly depleted, moderately depleted and slightly depleted. The slightly depleted samples (which are mainly but not exclusively aphyric basalts) show high log 10 f O 2 values (QFM À1.0, where QFM is quartz-fayalite-magnetite). Highly depleted samples, which are mainly olivine-phyric basalts, have low log 10 f O 2 values (QFM À3.5). On the basis of mixing calculations between La/Lu and 87 Sr/ 86 Sr we favour models linking the correlation between LREE abundances and log 10 f O 2 to mantle heterogeneity rather than contamination by oxidized, LREE-rich crustal fluids. SNC chemistry in general reflects the Fe-rich mantle of Mars (which contains twice as much FeO as the Earth's mantle), the late accretion of chondritic material into the mantle, and possibly the presence of a plagioclaserich magma ocean, which acted to variably deplete the mantle in Al. The high FeO contents of the SNC melts are associated with high melt densities (allowing the ponding of large magma bodies) and low viscosities, both of which are consistent with the large scale of many observed martian lava flows.Of the approximately 30 000 currently known meteorites, 32 originated on Mars. The martian meteorites are also called the SNC group after three of its members: Shergotty, Nakhla, Chassigny. They are known to form a distinct group of meteorites from a single parent body on the basis of their relatively differentiated mineralogy and chemical compositions; oxygen isotope compositions that are related to each other by mass fractionation (e.g. Clayton & Mayeda 1996); high oxidation state for meteorites (log f O 2 between QFM (quartz-fayalite-magnetite) and IW (iron-wüstite); e.g. Herd 2003) and notably large range of crystallization ages (165 Ma to 4.5 Ga; Nyquist et al. 2001a).It is the crystallization ages that first led to wide acceptance that this meteorite group was derived from a large, slowly cooled planet, Mars (e.g. McSween et al. 1979;Wood & Ashwal 1981). However, suggestions that some meteorites might be derived from Mars can be traced back further (e.g. Wänke 1968). Papanastassiou & Wasserburg (1974) noted that one of the SNC meteorites (Nakhla) must have been derived from an (unspecified) planetary object with some affinities to the Earth that had undergone differentiation after 3.6 Ga. The definitive link to Mars was made through comparing the composition of gases within the shock-melted glass of shergottites with the composition of the martian atmosphere determined by the Viking landers (Bogard & Johnson 1983).The SNCs have a range of basaltic and ultramafic mineral as...

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“…1) and have been described as olivine-phyric shergottites or picritic shergottites (Gnos et al 2002;Goodrich 2003). This includes lithology A of EETA79001.…”

Section: Olivine-rich Shergottitesmentioning

confidence: 99%

The SNC meteorites: basaltic igneous processes on Mars

Bridges

Warren²

2006

JGS

135

128

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“…size = 1.5mm) embedded in a fine-grained (ave. max. size = 0.3mm) groundmass of maskelynite and pigeonite [36], are comparable to those of SaU 005/008/051 and they are considered as pairs [40]. Moreover, both pieces display the same shock stage (S5) associated with shock twining, mosaicism and local oxidation in olivine [36].…”

Section: Sau 005+pairings Find History and Review Of Published Datamentioning

confidence: 66%

Review of the Sayh al Uhaymir (SaU) 005, Plus Pairings, Martian Meteorite from Al Wusta, Oman

Ali

Nasir

Jabeen

et al. 2017

SQU Journal for Science

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Al Wusta is a desert area in the Sultanate of Oman which is famous due to the discovery of a number of Martian and Lunar meteorites since the start of the present millennium. According to the Meteoritical Bulletin database, 137 approved Martian meteorites have been found worldwide, including 17 from Oman (4 from Zufar, 13 from Al Wusta region). Interestingly 11 finds in the last 15 years have been of Sayh al Uhaymir (SaU) 005 and its pairings. These finds (estimated mass = 11.2 kg) are linked to 10 search expeditions carried out between November 26, 1999 and March 2, 2014 by the Swiss group from the University of Bern and several anonymous meteorite hunters. The bulk of these meteorites (~97%) is in the possession of anonymous collectors, negatively affecting Oman's natural heritage and denying further research opportunities, given their associated scientific value.SaU 005 and its pairings belong to the shergottite group of the Shergotty-Nakhla-Chassigny (SNC) meteorites, originating from various depths within the Martian mantle. We discuss the recently published oxygen isotope data of bulk and mineral fractions of SaU 008 recovered during the very first expedition in 1999 in Petrographic and mineralogical data of SaU 005 and other pairings published in the Meteoritical Bulletin are compiled, and it is noted that all the meteorites are identical and are likely paired. The story behind these rare extra-terrestrial specimens demands a local meteorite museum and preliminary testing laboratory at Sultan Qaboos University (SQU) to protect this treasure trove of Omani heritage. Keywords

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“…It has been observed that all phosphate grains present in SaU 094 and SaU 150 meteorites, paired with SaU 005/008, represent merrillite, and no apatite has been found [69,101]. However, petrographic observations revealed that both merrillite and apatite are present in DaG 476 [101]. Apatite observed in DaG 476 have patchy texture that is consistent with anhedral growth on the rims of other late-stage minerals, such as merrillite and pyroxene [46].…”

Section: Petrogenetic Relationshipmentioning

confidence: 86%

“…Shergottites contain trace quantities of apatite that is relatively more abundant in the enriched ones compared to their depleted counterparts [46]. It has been observed that all phosphate grains present in SaU 094 and SaU 150 meteorites, paired with SaU 005/008, represent merrillite, and no apatite has been found [69,101]. However, petrographic observations revealed that both merrillite and apatite are present in DaG 476 [101].…”

Section: Petrogenetic Relationshipmentioning

confidence: 92%

Oxygen Isotope Thermometry of DaG 476 and SaU 008 Martian Meteorites: Implications for Their Origin

et al. 2018

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Abstract:We report the equilibration temperatures derived from the oxygen isotope thermometry of pyroxene-olivine pair from the Dar al Ghani (DaG) 476 (1200 +105/−90 • C) and Sayh al Uhaymir (SaU) 008 (1430 +220/−155 • C) meteorites showing a difference of over 200 • C at the face values. Regardless of the large associated uncertainties, contrasting geochemical and isotopic characteristics such as oxygen fugacities, hydrogen isotopic compositions (referred to as the D/H ratios), olivine abundances, presence of merrillite and/or apatite, and their chlorine contents between the two meteorites are observed in the literature. These opposing features lend support to the idea that the relative difference observed in the estimated temperatures is probably real and significant, thus providing insights into the Martian mantle magmatism. Based on our temperature estimation and previous magmatic models, we propose that SaU 008 could have been originated from a deeper depleted mantle source. However, DaG 476 may have been produced by the partial melting of the entrained pockets of the depleted mantle similar to that of the SaU 008's source at a relatively shallower depth. Both meteorites erupted as a relatively thick lava flow or a shallow intrusion at approximately the same time followed by a launch initiated by a single meteoritic impact 1.1 million years (Ma) ago.

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Sayh al Uhaymir 094: A new martian meteorite from the Oman desert

Cited by 53 publications

References 33 publications

The SNC meteorites: basaltic igneous processes on Mars

The SNC meteorites: basaltic igneous processes on Mars

Review of the Sayh al Uhaymir (SaU) 005, Plus Pairings, Martian Meteorite from Al Wusta, Oman

Oxygen Isotope Thermometry of DaG 476 and SaU 008 Martian Meteorites: Implications for Their Origin

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