The oxygen isotope composition of Almahata Sitta

Rumble, Douglas; Zolensky, M. E.; Friedrich, J. M.; Jenniskens, Peter; Shaddad, Muawia H.

doi:10.1111/j.1945-5100.2010.01099.x

Cited by 39 publications

(59 citation statements)

References 18 publications

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“…2) were constrained to δ 18 O = 8.1 ‰, δ 17 O = 3.2 ‰, Δ 17 O = −1.06 ‰ and δ 18 O = 8.0 ‰, δ 17 O = 3.2 ‰, Δ 17 O = −1.04 ‰ (for details, see SI Appendix). They fall in the range of other ureilites, including those from Almahata Sitta (10,11,15,16), but at the 16 O-poor end of the range of oxygen isotopes in ureilites, which is the more common oxygen isotope composition found among ureilites.ALM-A ( Fig. 1; see SI Appendix, Tables S1− S3 and Figs.…”

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confidence: 99%

Trachyandesitic volcanism in the early Solar System

Bischoff¹,

Horstmann²,

Barrat

et al. 2014

Proc. Natl. Acad. Sci. U.S.A.

102

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Volcanism is a substantial process during crustal growth on planetary bodies and well documented to have occurred in the early Solar System from the recognition of numerous basaltic meteorites. Considering the ureilite parent body (UPB), the compositions of magmas that formed a potential UPB crust and were complementary to the ultramafic ureilite mantle rocks are poorly constrained. Among the Almahata Sitta meteorites, a unique trachyandesite lava (with an oxygen isotope composition identical to that of common ureilites) documents the presence of volatile-and SiO 2 -rich magmas on the UPB. The magma was extracted at low degrees of disequilibrium partial melting of the UPB mantle. This trachyandesite extends the range of known ancient volcanic, crust-forming rocks and documents that volcanic rocks, similar in composition to trachyandesites on Earth, also formed on small planetary bodies ∼4.56 billion years ago. It also extends the volcanic activity on the UPB by ∼1 million years (Ma) and thus constrains the time of disruption of the body to later than 6.5 Ma after the formation of Ca-Al-rich inclusions.A large number of planetary embryos, tens to hundreds of kilometers in size, accreted within the early Solar System. In some of these embryos, internal heating triggered melting and differentiation, giving rise to a varied suite of lithologies as documented by the achondritic meteorites. Planetary crustal growth occurs via both volcanic eruptions and plutonic intrusions. Constraining these processes and the diversity of crustal materials that formed the outermost solid shell of planetary bodies is crucial for understanding Solar System planetary processes and evolution.Ureilites are among the most common achondrites and represent remnants of the mantle from a planetary body from which magmas have been extensively extracted (1−4). Several details of ureilite petrogenesis (e.g., the mode of melt extraction) remain controversial (e.g., refs. 1 and 2) because crustal rocks from the ureilite parent body (UPB) have not yet been discovered. Although tiny remnants of feldspathic and felsic melts from ureilitic breccias have been interpreted as UPB basalts or products of partial melting of plagioclase-bearing cumulates (e.g., refs. 5 and 6), it is generally assumed that the complementary melts were lost to space during explosive eruptions (e.g., refs. 7-9).A unique opportunity to gain new insights into ureilite petrogenesis was provided by the polymict asteroid 2008 TC 3 that impacted our planet October 7, 2008, in the Nubian Desert, Sudan, containing various ureilitic and ureilite-related fragments (10, 11). Among its remnant fragments collected in the strewn field, collectively named the "Almahata Sitta" meteorites, the sample ALM-A (Almahata Sitta trachyandesitic meteorite) was recovered (12). ALM-A weights 24.2 g and is covered with a greenish and shiny fusion crust (Fig. 1).The ALM-A sample described here is the only SiO 2 -rich, rapidly cooled volcanic rock among the meteorites in our collections. This rock is textura...

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confidence: 99%

Trachyandesitic volcanism in the early Solar System

Bischoff¹,

Horstmann²,

Barrat

et al. 2014

Proc. Natl. Acad. Sci. U.S.A.

102

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“…The few data points showing a scatter in ∆ 17 O values (Figure 2) are likely to be associated with either terrestrial weathering (assuming that samples were analyzed without acid-treatment given the absence of such details reported in the literature) or due to analytical artifacts in δ 17 O measurements ( 17 O abundance = 0.04%; see Figure 1). However, recently researchers [19] have analyzed SNC meteorites and they have found no significant variation in ∆ 17 O values between the untreated and acid-treated samples. Their data did not support the idea of scatter in ∆ 17 O due to a weathering phenomenon.…”

Section: Oxygen Isotope Data Of Snc Meteorites From the Sultanate Of mentioning

confidence: 99%

“…However, recently researchers [19] have analyzed SNC meteorites and they have found no significant variation in ∆ 17 O values between the untreated and acid-treated samples. Their data did not support the idea of scatter in ∆ 17 O due to a weathering phenomenon. However, it is noted that the data of acid-treated samples are skewed towards lower values.…”

Section: Oxygen Isotope Data Of Snc Meteorites From the Sultanate Of mentioning

confidence: 99%

“…If weathering is non-terrestrial, e.g., having occurred on the surface of Mars, the trend will be different as evidenced by [26] from the Lafayette meteorite. They reported heavier δ 18 O and higher ∆ 17 O values for Low-T mineral (e.g., Iddingsite) formed on the surface of Mars. Antarctica has a large population of meteorites which have remained preserved under the ice cover for extended periods of time.…”

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confidence: 99%

“…Offsets in oxygen isotope ratios relative to the TFL are used to characterize meteorite groups (Figure 1 [20]) to study the unique oxygen isotope signatures of meteorites. However, Miller [21] proposed the use of prime notation (′ 17 O, ′ 18 O), which takes into account the linear function relationship between  17 O and  18 O for a sample measured with respect to a reference, instead of the conventional approximation of a power law function. Construction of the TFL, based on various types of terrestrial materials, is a pre-requisite to conduct geochemical and cosmochemical studies in a stable isotope laboratory.…”

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confidence: 99%

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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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