Anand, M.

Franchi, I. A.

Potts, N. J.

Tartèse, R.

English

Open Research Online (The Open University)

Open Research OnlineThe Open University’s repository of research publicationsand other research outputsUnderstanding the Chlorine Isotopic Compositions ofApatites in Lunar BasaltsConference or Workshop ItemHow to cite:Potts, N. J.; Tarte`se, R.; Franchi, I. A. and Anand, M. (2015). Understanding the Chlorine Isotopic Compositions ofApatites in Lunar Basalts. In: 46th Lunar and Planetary Science Conference, 16-20 Mar 2015, The Woodlands, TX,USA.For guidance on citations see FAQs.c© [not recorded]Version: Version of RecordCopyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyrightowners. For more information on Open Research Online’s data policy on reuse of materials please consult the policiespage.oro.open.ac.ukUNDERSTANDING THE CHLORINE ISOTOPIC COMPOSITION OF APATITES IN LUNAR BASALTS.  N. J. Potts1,2*, R. Tartèse1, I. A. Franchi1, M. Anand1,3.  1Department of Physical Sciences, The Open University, Milton Keynes, UK. (*nicola.potts@open.ac.uk). 2Faculty of Earth and Life Sciences, VU University Amsterdam, Amsterdam, NL. 3Department of Earth Sciences, The Natural History Museum, London, UK.    Introduction: On Earth δ37Cl = ~0 ± 5 ‰ [1]. For lunar rocks elevated δ37Cl values of up to 35 ‰ have been reported in apatites [1,2]. The initial study inter-preted the elevated δ37Cl in lunar rocks as a result of metal chlorides degassing in low-H2O environments [1]. Additional data [3,4] have shown high-δ37Cl val-ues in samples with apatite containing appreciable amounts of H2O (>2000 ppm). Metasomatism is thought to have fractionated Cl isotopes toward heavy δ37Cl values in sample 79215 [2]. This process, how-ever, is not thought to be widespread on the Moon and cannot account for the fractionation seen in other sam-ples for which data are available, particularly mare basalts. Here we report preliminary measurements of δ37Cl in apatites from lunar impact “melt rock” sample 14073,9. Results are compared with literature δ37Cl data on lunar apatites to evaluate the effects impact processes may have had on δ37Cl values. We then ex-plore a potential scenario of the elevated δ37Cl signa-ture of the Moon. Figure 1: BSE image of 14073,9. Blue spots (not to scale) correspond to NanoSIMS analysis locations for apatite #12.  Sample petrogenesis: 14073 was initially classi-fied as a KREEP basalt due to its high REE content [5]. There are similarities in trace element abundances between 14073, and Apollo 14 soils and breccias. This, along with high Ni and Ir contents and the presence of Fe-Ni-P-S melt globules, led to its description as a “melt rock” [6].  It consists of euhedral plagioclase laths (~50% modal abundance) with interstitial anhe-dral pyroxenes (~25% clinopyroxene; ~20% orthopy-roxene) with minor ilmenite (~2%), and a late-stage mesostasis [7]. The mesostasis regions of 14073,9 are composed of apatite, merrillite, fayalite, sanidine, and K-Ba-rich glass. Methods: Apatite grains were identified, initially using SEM-derived X-ray maps and  BSE images, fol-lowed by 16O1H and 35Cl secondary ion images using the real-time imaging mode of the Cameca NanoSIMS 50L ion probe. For NanoSIMS measurements, a Cs+ primary beam of 560 pA with an accelerating voltage of 16 kV was rastered on the sample surface over 25  25 μm areas for 1 minute to pre-sputter and clean the sample surface. Areas of 8  8 μm were then rastered for a further minute with a 90 pA beam current. Final-ly, analyses were carried out on 4  4 μm areas with a 40 pA beam current. Secondary ions of 16O1H, 18O, 28Si, 35Cl, 37Cl, and 40Ca19F were collected simultane-ously on electron multipliers for ~7 minutes. Cl and OH abundances were calibrated using the 35Cl/18O and 16O1H/18O ratios measured on reference apatites stand-ards [8]. Abundance errors are low for both Cl (30 – 60 ppm) and H2O (17 – 22 ppm). Due to its high abun-dance and high ionisation efficiency, F abundances could not be measured directly on an electron multipli-er and were calculated by difference (F = (1-(Cl+OH)) apfu). The same standards used to calibrate abundanc-es were used to correct measured 37Cl/35Cl ratios for instrumental mass fractionation (IMF). The 37Cl/35Cl ratios are given here in the standard delta notation cali-brated against the 37Cl/35Cl ratio for Standard Mean Ocean Chloride (SMOC). Errors shown are 2σ.  Results:  Four δ37Cl values, from 3 apatites, are re-ported here. The apatite grain (#12) in which 2 anal-yses were carried out, is shown in Figure 1. δ37Cl val-ues within this grain are appreciably different with values of +5.0 ± 2.7 ‰ and +14.8 ± 2.6 ‰, demon-strating a large variation in δ37Cl values within a single apatite grain. The Cl concentrations measured at the two spots vary by more than a factor of 2 (1812 and 4006 ppm, respectively), and broadly similar H2O con-tents of 782 and 1102 ppm, respectively. Figure 2 shows that there is no obvious relationship between δ37Cl and H2O content in the analysed apatites, while there is a positive correlation between Cl content and δ37Cl (R2 = 0.99). This may, however, be a reflection of the small variation in H2O content. In terms of δ37Cl vs. Cl concentration, apatites in 14073,9 plot within similar regions to basalts from [1,3] and an isolated apatite grain found within the matrix of lunar meteorite 2077.pdf46th Lunar and Planetary Science Conference (2015)breccia Northwest Africa (NWA) 4472 [4]. Cl concen-trations in apatites from [1] are all higher than those measured in [3] and this study. The apatites from [1] also have the highest δ37Cl value measured from mare basalts thus far. The majority of Cl concentrations from [3] are lower than values measured in this study.   Figure 2: δ37Cl versus Cl (yellow squares) and H2O (blue circles) concentrations for apatites in 14073,9.  Discussion: There appears to be no relationship be-tween the bulk geochemistry of the basalts and δ37Cl values in the literature data. As the results of 14073,9 are indistinguishable from mare basalts, impact pro-cesses do not appear to have influenced Cl concentra-tions or δ37Cl values in this sample. Further data, how-ever, are required to determine whether this sample retains initial magmatic signatures. The results of [3] showed the variability of δ37Cl values within a lunar sample. This demonstrated that multiple apatites should be measured when investigat-ing Cl isotopes. The data from the current study show that δ37Cl values and Cl concentrations can vary great-ly within one grain over a 10 µm distance. Multiple analyses, preferably both concentration and isotopic measurements on the same spot, from a number of apatites per sample are desirable for an accurate as-sessment of indigenous Cl isotope signatures.  Apatite data from 14073,9 and [1] appear to show a general trend between increasing Cl concentrations and increasing δ37Cl values (R2 = 0.92). More data are re-quired to quantify potential trends between Cl concen-tration and δ37Cl values. If these trends are robust then a process which simultaneously increases Cl concen-tration and 37Cl is required [or vice versa]. Based on the data presented in Figure 1, this process does not appear to be strongly linked to changes in apatite water contents. Preferential degassing of the lighter 35Cl would reduce the Cl concentration and, as such, the opposite trend would be expected if this were the main process affecting Cl isotope fractionation [9]. Observa-tions from [3] indicate a potential mixing trend be-tween δ37Cl-elevated highlands samples and relatively δ37Cl-depleted lunar basalts.  Isotopically heavy δ37Cl values and high Cl con-centrations in apatites from lunar highlands samples could represent initial Moon Cl values. A process, however, that enriches Moon-forming material in heavy 37Cl relative to the Earth would be required for this scenario (based on the assumption of the Moon being formed from BSE-type material). A study on Earth’s Cl depletion relative to chondritic material [10] suggests preferential loss of heavy halogens during planetary accretion as a possible scenario. Large im-pactors, such as a giant Moon-forming impact [10], result in preferential loss of a Cl-rich veneer from Earth. During accretion of the Moon, and subsequent outgassing, the lighter 35Cl would be preferentially lost to space [1] which would also significantly reduce the bulk-Cl content of the Moon. A similar hypothesis was initially discarded by [1] from a lack of supporting evidence from other volatiles such as K. This volatile enrichment in the Moon, however, would be expected for only the heavy halogens such as Cl, I, and Br [10].  It is unknown, however, what process(es) could further fractionate Cl isotope signatures of mare source regions as apatites in mare basalts appear to have rela-tively lighter Cl isotope signatures compared to the highlands samples. A better understanding of other petrological influences in modifying the Cl isotopic signatures of lunar samples is required to further ad-dress this issue. Ongoing work aims to acquire addi-tional data for δ37Cl from analyses of multiple grains within a sample to provide further insight into any var-iability of δ37Cl values in mare basalts as per their geo-chemistry, age, depth burial, etc. These measurements will ultimately help improve our understanding of the significance of the heavy δ37Cl signatures of lunar apa-tites and their potential implications for the history of water in the lunar interior. Acknowledgements: We thank NASA CAPTEM for allocation of Apollo samples. This work was funded by an STFC Studentship awarded to NJP and research grant to MA (Grant no. ST/I001298/1). Francis McCubbin is thanked for providing apatite standards.  References: [1] Sharp, Z.D. et al. (2010) Science, 329, 1050-1053. [2] Treiman, A.H. et al. (2014) Am. Min. 99, 1860-1870. [3] Boyce, J.W. et al. (2013) LPSC, 44th, #2851. [4] Tartèse, R. et al. (2014), MaPS, 49, 2266-2289. [5] El Goresy, A. et al. (1971) EPSL, 13, 121-129. [6] Schonfed, E., Meyer, C. (1972) 3rd Lunar Sci. Conf. 1681-1691. [7] Gancarz, A.L., et al. (1971) EPSL, 12, 1-18. [8] McCubbin F.M. et al. (2012) Geol., 40, 683-686. [9] Hauri E.H. et al. (2015) EPSL,409,252-264. [10] Sharp, Z.D., et al.. (2013) EPSL, 369-370, 71-77.  2077.pdf46th Lunar and Planetary Science Conference (2015)

Understanding the Chlorine Isotopic Compositions of Apatites in Lunar Basalts

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