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Igneous Petrology and Geochemistry of the Tissint Meteorite

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Igneous Petrology and Geochemistry of the Tissint Meteorite 46th Lunar and Planetary Science Conference (2015) 1267.pdf IGNEOUS PETROLOGY AND GEOCHEMISTRY OF THE TISSINT METEORITE. J.B. Balta1-2, M.E. Sanborn3-4, A. Udry1-5, M. Wadhwa3 and H.Y. McSween2. 1Planetary Geoscience Institute, University of Tennessee, Knoxville TN. 2University of Pittsburgh, Pittsburgh PA, [email protected]. 3Arizona State University, Tempe AZ. 4UC Davis, Davis CA. 5UNLV, Las Vegas, NV. Introduction: Since its fall and recovery in the dance of largest crystals compared to what simple Moroccan desert during 2011, the Tissint meteorite has crystallization would produce [6] as would occur with been the subject of a number of studies, including stud- assembly of glomerocyrsts. Olivine REE abundances ies of its shock phases, melt inclusions, and hydrogen are low, below detection limits in many cases, with no isotopes [1-4]. However, there has yet to be a complete sign of upturn in the LREE pattern associated with summary of the the Tissint meteorite’s origin from a alteration or hot-desert weathering [7]. perspective of its igneous petrogenesis. Tissint is an olivine-phyric shergottite, the Pyroxenes: Pyroxenes make up 50-52% of the two thin class of meteorites with parent melt compositions clos- sections, similar to the abundance in other olivine- est to equilibrium with the martian mantle, and thus phyric shergottites. Pyroxene compositions also over- understanding its igneous petrogenesis will give new lap those in other olivine-phyric shergottites, continu- geochemical constraints about the martian mantle and ously varying between pigeonite and augite with Fe- generation of shergottite magmas. To characterize this rich overgrowths. Minor elements, including Ti and igneous petrogenesis and place Tissint in the context of Al, vary significantly and are correlated with geochem- the other shergottites, we conducted a detailed analysis ical properties such as Mg # that suggest coupling to of two thin sections of the Tissint meteorite obtained the crystallization sequence. Minor elements in pyrox- from Arizona State University’s Center for Meteorite ene also overlap with those observed in other previous Studies collection. We characterized the sample shergottites including depleted shergottite QUE 94201 through petrography, backscattered electron imaging, and intermediate shergottite EETA 79001A [8-9]. Py- and Electron Microprobe analyses at the University of roxene trace element abundances increase from pi- Tennessee, and secondary ion mass spectrometry at geonite/Mg-rich cores to augite/Fe-rich rims and show Arizona State University. small Eu anomalies that increase slightly from pigeon- We find that Tissint occupies a unique petro- ite to augite. No upturn in the LREE pattern is ob- logic niche in the shergottites, distinct chemically from served in Tissint pyroxenes. the other martian meteorites. These distinctive proper- ties include both its highest-Mg # olivine falling in a Maskelynite: All plagioclase in Tissint has been con- previously-unsampled range, the largest range in oli- verted to maskelynite during shock. Maskelynite made vine compositions observed in a shergottite, and a up 20-22% of the analyzed thin sections. Maskelynite unique crystalization path with olivine on the liquidus varies from An68Ab42Or1 to An47Ab48Or5, comparable before chromite. It shows a highly-reduced oxygen to shergottites such as QUE 94201 and EETA 79001A fugacity consistent with other depleted shergottites, but in their An-rich end member but with a slightly more its trace element abundances overlap those observed in Ab-rich end-member [9-10]. Maskelynites are REE- more oxidized or intermediate shergottites. It may rep- depleted relative to other shergottites including some resent a more olivine-rich and thus closer-to-primary depleted shergottites, but are overall similar to DaG version of basaltic shergottite QUE 94201. 476/489 [11]. Eu anomalies in Maskelynite are smaller than those observed in depleted shergottites including Olivine: Olivine in Tissint varies from Mg# 81 to 29, DaG 476/489 or in intermediate shergottite EETA including the most Fe-rich rims found in any olivine- 79001A, but are larger than those observed in enriched phyric shergottite. Olivine cores are close to homoge- shergottite LAR 06319 [12]. neous between Mg # 80-81; large olivines contain melt inclusion trails implying they are glomerocrysts and Minor phases: Merrillite is the dominant phosphate in likely resided inside an active magmatic system before Tissint; our investigations did not locate any apatite in entrainment. The two examined sections contained these two thin sections although it has been previously 27% and 24% olivine respectively and have accumu- reported [13]. Merrillites range from 2.4 to 4.9 wt. % lated 7-10% olivine beyond what could form from the FeO, making them among the more Fe-rich phosphates Tissint parental magma, a number similar to that ob- observed in shergottites. This phase is the main REE served in several olivine-phyric shergottites [5]. Crys- carrier in Tissint. Merrillite REE abundances parallel tal Size Distribution (CSD) measurements show nega- those of other depleted and intermediate shergottites tively-sloped arc shapes, consistent with overabun- but average REE contents are slightly elevated even 46th Lunar and Planetary Science Conference (2015) 1267.pdf relative to intermediate shergottite EETA 79001A [8]. presented measurements of Tissint [13]). These calcu- No upturn in the LREE pattern is observed in Tissint lations also show that both early-crystallized pyrox- merrillites. enes and late-crystallized merrillites could be formed Oxide minerals vary in composition from from a single parental magma, implying no assimila- chromite through titanomagnetite to magnetite and tion of any enriched component during crystallization. ulvöspinel, with the latter having cocrystallized with No upturn in the LREE pattern is observed in pyrox- ilmenite. A full compositional trend from Cr-rich to Ti- enes although this was previously reported in Tissint Fe rich oxides is present in Tissint. Notably, no coarse- melt inclusions [4], implying a post-trapping origin the grained chromites were observed as inclusions in oli- LREE pattern in those inclusions. vine phenocrysts unless also accompanied by a melt- The REE abundances in the Tissint bulk rock gen- pocket. Sulfides are present and are uniformly pyrrho- erally overlap with those of shergottites classified as tite, as found in other shergottites. intermediate based on isotopic compositions and oxy- gen fugacities, reinforcing previous suggestions of Implications for Magma Evolution: Olivine was the similarities between REE abundances of these two first mineral to crystallize from the Tissint parent groups [19]. Tissint’s bulk rock REE pattern also par- magma. Olivine as the liquidus mineral implies crys- allel that of depleted basaltic shergottite QUE 94201, tallization began at pressures below the multiple- but with higher REE abundances in QUE 94201 con- saturation point for olivine and pyroxene; e.g., below sistent with its lack of olivine [8]. ~1.2 GPa [14]. Tissint is the 3rd olivine-phyric sher- Oxygen fugacities calculated using the olivine- gottite to contain olivines with Mg # > 80; Yamato pyroxene-spinel assemblage give values in the range 980459 and NWA 5789 contain olivines with Mg # ~ QFM -3.5 to -4.0 depending on choice of mineral 85 [15-16] and thus the most Mg-rich olivines from composition [20]. Application of the Eu oxybarometer Tissint fall into a previously unsampled range. The to pyroxene cores [21] gives fO2 of QFM -2.4, slightly CSD pattern of Tissint olivines resembles that of en- more oxidized than suggested by the mineral assem- riched shergottite LAR 06319 [12], implying that oli- blages but within the 2SD error of the calibrations. vine crystallization followed by storage in an active Tissint is therefore among the most reduced of the magmatic system is likely a common process in sher- shergottite meteorites, comparable to other depleted gottite magmatism across both the enriched and de- shergottites such as SaU 005 [22] and QUE 94201, and pleted end-members. Chromite crystallization in could represent a more olivine-rich, parental version of Tissint was delayed until after significant olivine crys- basaltic shergottite QUE 94201. tallization, a result not previously described in sher- gottites. Olivine grains were held together, either in a References: [1] Baziotis I.P et al. (2013) Nature, 4, cumulate pile or on the edges of a magma chamber, 1404-1408 [2] Brennecka G.A. et al. (2014) MAPS where multiple grains fused together into glomero- 49(3), 412-418 [3] Mane P. et al. (2013), LPSC XLIV, crysts and olivine compositions homogenized. After #2220 [4] Peters T.J. et al. (2014), LPSC XLV, #2405 re-entrainment of these olivines into the final host [5] Filiberto J. and Dasgupta R. (2011) EPSL 304, 527- magma, chromite, lower-Mg # olivine, and orthopy- 537 [6] Udry A. et al. (2013), LPSC XLIV, #1719. [7] roxene/pigeonite began co-crystallizing, with plagio- Crozaz G. and Wadhwa M. (2001), GCA 67, 4727- claise crystallization beginning shortly thereafter. Py- 4741. [8] Wadhwa M. et al. (1994), GCA 58, (4213- roxene minor elements suggest depletion of Ti and Al 4229) [9] Wadhwa M. et al. (1998), MAPS 33, 321- in the melt during crystallization and possibly decreas- 328. [10] McSween H.Y. and Jarosewich E. (1983), ing pressure [17], although there is no evidence of dis- GCA 47, 1501-1513. [11] Wadhwa M. et al. (2001), solution of olivine or pyroxene as might be expected MAPS 36, 195-208. [12] Balta J.B. et al. (2013), during decompression [18]. Tissint shows evidence of MAPS 48, 1359-1382. [13] Chennaoui Aoudjehane, H. an extended crystallization interval, producing iron- et al. (2012) Science 338, 785-788 [14] Balta J.B. and rich rims on olivines and Fe-Ti rich oxide phases. McSween H.Y. (2013), JGR Planets 2013JE004461 Measured trace element abundances in pyrox- [15] Ikeda Y. (2004), Ant. Met. Res. 17 (35-54). [16] enes and merrillites were used along with known REE Gross J. et al. (2013), MAPS 46, 116-133 [17] Filiberto partition coefficients to reconstruct the REE abundanc- J.
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