Cl in the Early Solar System Jeffrey Williams

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Summer 7-30-2016 Cl in the Early Solar System Jeffrey Williams

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2 CL IN THE EARLY SOLAR SYSTEM

4 BY

6 Jeffrey Thomas Williams

7 B.S. Geology, Florida State University, 2013

12 THESIS

13 Submitted in Partial Fulfillment of the

14 Requirements for the Degree of

15 Master of Science

16 Earth and Planetary Science

17 The University of New Mexico

18 Albuquerque, New Mexico

19 July, 2016 i

6 Dedication

7 “Honesty is Simplicity”

10 I dedicate this work to my partner in life, Lacy Catherine Saenz. Without your support,

11 encouragement, and guidance, I would not be the man I am today. I will always love and

12 support you.

18 ii

2 Acknowledgements

4 I would like to whole heartedly acknowledge the great support and opportunity I have

5 been given by my advisors Dr. Charles Shearer and Dr. Zachary Sharp. I am very

6 appreciative for everything I am taking away from this experience.

7 I would also like to thank Dr. Francis McCubbin. Your guidance through this process

8 has had a large impact on my direction as a professional and as a person. You are a great

9 asset to the scientific community and to the next generation.

10 Lastly, I would like to thank my parents Pamela and John Williams. Your love and

11 care have given me greater opportunity than I could have imagined. You are both beautiful

12 people and I am proud to have you as my parents.

19 iii

1 TABLE OF CONTENTS

3 Introduction………………………………………………………………………………1

5 Chapter 1: The Chlorine Isotopic Composition of Martian Meteorites 1.

6 Chlorine Isotope Composition of Martian mantle and crustal reservoirs and their

7 interactions……………………………………………………………………………… 4

9 Chapter 2: Tracking Cl in Primitive Ordinary Chondrites:

10 Evidence for HCl-Clatherate Formation in the Solar Nebula……………………….40

12 Appendix 1:H, N and C Isotopic and Concentration Measurements of Selected

13 Chondrites…………………………………………………………………...... 72

15 References……………………………………………………………………………….76

16 1

2 Introduction

3 The early solar nebula is thought to have been a turbulent disk of dust and gas. An unknown

4 mechanism caused the disk to collapse, such as a nearby super nova. This collapse led to high

5 temperatures and high particle densities at the mid-plane of the disk. An unknown mechanism

6 caused the temperature in local area to become hot enough to cause some material to melt –creating

7 the first igneous material of the solar system. These melt spherules, called chondrules, cooled and

8 accreted together with dust and ice to form larger bodies called chondrites. Once the chondritic

9 bodies were of sufficient size, and enough 26Al decayed which was the primary heat source for

10 planetary interiors, these bodies began to melt and undergo differentiation (core, mantle and crust

11 formation) and become planetesimals. These planetesimals were the building blocks for all of the

12 planets we currently have today. Our window into understanding these early solar system

13 processes come from our collection of meteorites.

14 The study of meteorites has led to many challenges in fully understanding nebular processes.

15 The identification of a mechanism for volatile element incorporation has remained a core problem.

16 It is unlikely that many volatile elements were initially incorporated into chondrules because of

17 the high temperature of formation. Further, there is little direct evidence for volatile incorporation,

18 i.e. condensing phases identification. Therefore, it has been a long prevailing idea that many

19 volatile elements were incorporated into the parent bodies post-accretion, mostly through fluids.

20 These process are difficult to identify. However, understanding volatile element incorporation in

21 chondritic bodies is paramount in the identification of volatile sources for the terrestrial planets. 2

1 Of all the volatile elements, the halogen group is of particular interest. Halogens, such as Cl

2 and F, are in relatively high concentration in many chondritic bodies, yet show high variability

3 (between <100 ppm to 700ppm Cl across the chondrite groups). These differences may reflect

4 either, or a combination of, different reservoir conditions, incorporation mechanisms, and/or post-

5 accretion processing. Chlorine, however, is the focus of this study.

6 Chlorine has many unique chemical characteristics. It is strongly hydrophilic. It does not

7 exhibit appreciable isotopic fractionation at high temperatures, yet may fractionate significantly at

8 low temperatures. And it is also strongly incompatible in magmatic systems. Thus, Cl is useful as

9 a geochemical proxy for many systems. In the following chapters, this study will address the

10 behavior of Cl on Mars and in ordinary chondrites. To do so, Cl isotopic measurements will be

11 used in conjunction with in situ elemental mapping, and petrologic description of material.

12 Chapter 1 will explore the Cl isotopic variation on Mars through Martian meteorites. Mars

13 is a volatile rich body, and is enriched in chlorine relative to Earth by a factor of 3. The collection

14 of known Martian meteorites spans a large range of geologic conditions. These samples include

15 crustal regolith breccia, basaltic melts, and dunites. This work explores the differences in the Cl

16 isotopic composition and the Cl concentration of the mantle and the crust. These differences will

17 be used to assess Cl ability to trace crustal contamination. An unexpected outcome of this work is

18 the isotopically light values measured for the Martian mantle-like samples; implying Mars sourced

19 a different nebular reservoir than the Earth. By understanding Cl in the Martian mantle we can

20 then reassess Cl in the early solar system.

21 Chapter 2 looks at the Cl isotopic composition and host phases in the most pristine chondritic

22 meteorites (3.00s). NWA 8276, L 3.00, has been shown to be isotopically light with respect to CL. 3

1 This work finds that NWA 8276 is anomalous compared to other 3.00’s have near-Earth Cl isotopic

2 compositions. A detailed study using in situ microbeam techniques of LL 3.00 Semarkona found

3 some chondrules to have high Cl concentrations. This study will seek to identify the host phases

4 of Cl in these enriched chondrules, and provide a mechanism for incorporation. NWA 8276 was

5 also studied using in situ elemental mapping techniques in an effort to explain the difference in Cl

6 isotopic composition. Understanding Cl in the 3.00 ordinary chondrites is important as it is most

7 likely to represent the initial condition of Cl incorporation in the early solar nebula.

19 4

1 CHAPTER 1

2 The Chlorine Isotopic Composition of Martian Meteorites 1.

3 Chlorine Isotope Composition of Martian mantle and crustal reservoirs and their

4 interactions.

5 J.T. Williams1,2, C.K. Shearer1,3, Z.D. Sharp1,2, P.V. Burger1,3, F.M. McCubbin3,4, A.R. Santos1,3,

6 C.B. Agee1,3, K. D. McKeegan5

7 Submitted to Meteoritics and Planetary Science

8 Submitted July 30, 2015

10 1Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, NM,

11 87131, USA, [email protected]

12 2Center for Stable Isotopes, University of New Mexico, Albuquerque, NM, 87131, USA

13 3Institute of Meteoritics, University of New Mexico, Albuquerque, NM, 87131, USA

15 4NASA Johnson Space Center, Mailcode XI2, 2101 NASA Parkway, Houston, Texas 77058,

16 USA

18 5Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 94607,USA 5

Abstract

The Martian meteorites record a wide diversity of environments, processes, and ages. Much work has been done to decipher potential mantle sources for Martian magmas and their interactions with crustal and surface environments. Chlorine isotopes provide a unique opportunity to assess interactions between Martian mantle derived magmas and the crust. We have measured the Cl isotopic composition of 17 samples that span the range of known ages, Martian environments, and mantle reservoirs. The δ37Cl of the Martian mantle, as represented by the olivine-phyric shergottites, NWA 2737 (chassignite), and Shergotty (basaltic shergottite), has a low value of approximately -3.8‰. This value is lower than that of all other planetary bodies measured thus far.

The Martian crust, as represented by regolith breccia NWA 7034, is variably enriched in the heavy isotope of Cl. This enrichment is reflective of preferential loss of 35Cl to space. Most basaltic shergottites (less Shergotty), nakhlites, Chassigny, and Allan Hills 84001 lie on a continuum between the Martian mantle and crust. This intermediate range is explained by mechanical mixing through impact, fluid interaction, and assimilation-fractional crystallization.

1.0 Introduction

Chlorine has many unique chemical characteristics. Chlorine is a moderately volatile element and is strongly hydrophilic. It does not exhibit appreciable isotopic fractionation at high temperatures, but may fractionate significantly at low temperatures (Kaufmann et al. 1984; Sharp et al. 2007, 2013). Nearly half of Earth's Cl resides in the oceans and evaporites (Sharp and Draper

2013), and most reservoirs have minimal isotopic variability (Sharp et al. 2007). Cl is also strongly incompatible in magmatic systems, which has left the terrestrial mantle depleted with respect to

Cl (Sharp and Draper, 2013). 6

Mars is volatile rich and is enriched in chlorine relative to Earth by a factor of 3 (Dreibus and Wänke 1985; Keller et al. 2006; Filiberto and Trieman 2009; Taylor et al. 2010; Sharp and

Draper 2013). Remote sensing data indicate that the Martian surface has a high Cl concentration ranging from 0.2 to over 1.0 wt%, with an average of 0.49 wt% (Keller et al. 2006). These data also indicate that the highest Cl concentrations can be found in the equatorial region of the

Medusae Fossae Formation. This region has been subjected to prolonged volcanic activity, suggesting that volcanic degassing has made a significant contribution to the concentration of Cl at the Martian surface (Keller et al. 2006). In addition, Cl appears to be an important tracer for past surficial water because it is concentrated within topographic lows at the surface, presumably by evaporation of surficial waters in basins and craters (Tosca and McLennan 2006; Osterloo et al

2006, 2010). The reservoirs of this crustal chlorine, as determined by Martian meteorites and remote sensing observations, are apatite, NaCl, glass, amphiboles, sheet silicates, scapolite, chloride deposits, Cl-rich dust, and perchlorate (e.g. Bridges and Grady, 1999; Bogard et al. 2010;

Filiberto et al., 2014; Hecht et al., 2009; Keller et al. 2006; McCubbin et al. 2009, 2012, 2013, this issue; Osterloo et al. 2006, 2010; Sautter et al. 2006). The absence of plate tectonics on Mars

(Breuer and Spohn, 2003; Spohn et al., 2001) has kept the mantle isolated from the crust and has preserved distinct crustal and mantle reservoirs of Cl (McCubbin et al., this issue).

The crust of Mars has also experienced a high degree of alteration resulting from various weathering mechanisms (Chan et al. 2008; Jain et al. 2015; Carter et al. 2015) and has interacted with an atmosphere that is highly fractionated, isotopically (Bogard, 1997; Gillmann et al., 2011;

Pepin, 1994). Numerous studies have documented that atmophile isotopic systems such as Xe, Kr,

Ar, and H are fractionated in the atmosphere relative to the composition of the primitive Martian mantle (Owen et al. 1977; Becker and Pepin 1984; Marti et al. 1995, Bogard 1997; Mathew and 7

Marti 2001; Usui et al., 2015). The isotopic evolution of the Martian atmosphere is largely attributed to hydrodynamic escape and interaction with solar wind (Chassefière and Leblanc,

2004). However, with the exception of hydrogen, these elements are extremely atmophile and occur in low concentrations in Martian meteorites (e.g. Marti et al. 1995; Bogard 1997). The moderately volatile, lithophile, and hydrophile nature of Cl should allow it to be fractionated similarly to the atmophile elements on Mars yet still be incorporated into Martian surface materials.

Most Martian meteorites represent mantle-derived magmas that experienced varying degrees and types of interactions with the Martian crust and/or atmosphere (Wadhwa, 2001; Herd et al., 2002; Borg and Draper 2003; Symes et al., 2008; Papike et al. 2009; Shearer et al. 2013;

Peters et al. 2015), so they represent our best opportunity to simultaneously investigate the compositions of mantle, crustal, and atmospheric reservoirs on Mars. In many previous studies, differences in REE geochemistry, radiogenic isotopic systematics, and oxygen fugacity were used to differentiate between various geochemical reservoirs on Mars. The intent of this study is to extend our knowledge of martian geochemistry by determining the isotopic composition of Cl in a suite of Martian meteorites. The Cl isotopic data are interpreted within the context of previous studies on martian meteorite geochemistry and petrology to determine the Cl isotopic composition of the Martian mantle and crust, the origin of their Cl isotopic compositions, and the interactions among mantle and crustal reservoirs.

2.0 Analytical Methods

The distribution of Cl in Martian meteorites and Cl isotopic compositions of both individual phases and bulk meteorites were examined using electron probe microanalysis (EPMA), 8 secondary ion mass spectrometry (SIMS), and conventional gas source isotope ratio mass spectrometry. The Martian meteorites analyzed for this study are listed in Table 1. The petrography of the individual meteorite samples are discussed in detail in a companion manuscript (Sharp et al., this issue).

2.1 Electron probe microanalysis (EPMA) and imaging:

Thin sections of selected Martian meteorites were initially documented using backscattered electron (BSE) imaging on the JEOL JXA-8200 Superprobe electron microprobe at UNM. Once suitable areas were identified, wavelength dispersive X-ray maps were collected for Ca, P, Cl, and

F and energy dispersive maps were collected for Mg, Al, and Fe. Maps were generated using a 15 kV accelerating voltage, a 100 nA beam current, and a dwell time of 800 ms/pixel. These X-ray maps identified the distribution of Cl-bearing phases and potential targets for SIMS analyses.

Quantitative EPMA analyses were conducted on apatite and glasses using an accelerating voltage of 15kV, a beam current of 20 nA, and a spot size varying from 1-3 µm. Standards for the apatite point analyses consisted of a suite of C.M. Taylor Company mineral and synthetic standards, as well as select, in-house, mineral standards. Cl was standardized using an in-house Sodalite standard (Sharp et al. 1989). Stoichiometric constraints were used to determine the quality of the

EPMA analyses, and detection limits were calculated at the 3σ level.

2.2 Bulk Mass Spectrometry Analyses:

The method for bulk chlorine extraction and analysis used in this study are modified from

Eggankamp (1994). Samples are crushed to a fine powder and leached with 18MΩ H2O for a minimum of four days to remove water-soluble chlorine, which has a high likelihood of containing terrestrial contamination. There is potential for the water-soluble Cl, especially in falls, to contain 9 a Martian-crustal signature. However, due to the difficulty in distinguishing terrestrial Cl from

Martian crustal Cl, this work will focus only on the structurally bound Cl. The water-soluble

chloride is preserved and analyzed for δ Cl. After leaching, the samples are melted in an H2O vapor stream (Magenheim et al.1994). The structurally-bound chlorine is volatilized, carried by the H2O vapor stream, and re-condensed as chloride into solution. The aqueous chloride solution is reacted with nitric acid for 12 hours to volatilize any contaminant sulfur and then reacted with

AgNO3 to form AgCl(s). The AgCl is vacuum filtered using GF/F glass filter paper and dried at

80° C. The AgCl is reacted with excess CH3I in evacuated glass tubes at 80°C for 48 hours to quantitatively convert AgCl to CH3Cl. CH3I and CH3Cl contained in the sealed tube are released into a helium stream using a tube cracker. Next, the gasses are cryofocused using liquid nitrogen.

The gas is then passed through a custom made glass GC column at 85° C to separate CH3Cl from

CH3I. The purified CH3Cl is measured on a Delta XL plus mass spectrometer in continuous flow mode. The flow of gas is reversed as soon as the CH3Cl peak has been analyzed to avoid the introduction of CH3I into the mass spectrometer. The two CH3Cl peaks (mass 50 and 52) are integrated, and the ratio is taken relative to a calibrated internal standard. The long-term external reproducibility of δ37Cl is ± 0.25‰ based on analysis of an in house seawater standard (Sharp et al. 2007, 2010a, 2010b; Barnes et al. 2006; Selverstone et al. 2011). Concentrations are determined by measuring external standards that span a range of known concentrations during the analytical session. The integrated peak areas of each sample are then compared to the standards to quantify the Cl concentration.

In addition to a bulk rock analysis, a sub split of the meteorite Tissint was separated into two components consisting of glass in one and crystalline material, similar to the materials that comprise the other Martian meteorites, in the other. The glass separate was dominated by a martian 10 impact glass component (Aoudjehane et al., 2012), but it probably had a small igneous glass component as well. This sample was crushed and then handpicked under a microscope. The glass fraction of Tissint was leached in 18MΩ H2O for two weeks prior to further extraction to ensure all water-soluble Cl was leached (similar to Sharp et al., 2010a for the Apollo 17 picritic glass beads).

All Cl isotope measurements (classical mass spectrometry and secondary ion mass spectrometry) are reported in standard delta notation:

�� δ�� = − 1 ×1000 ��

The in-house standard used for chlorine isotope measurements is Carmel seawater, which we have measured and confirmed is indistinguishable from Standard Mean Ocean Chloride (SMOC), hence it has a value of 0‰ by definition (Kaufmann 1984).

2.3 Secondary Ion Mass Spectrometry Analysis:

In situ ion microprobe analyses were made on the large radius Cameca ims 1270 ion microprobe at UCLA using a Cs+ primary beam focused to ~10 - 20 µm following procedures outlined in Sharp et al. (2010a). Secondary ions were measured simultaneously for mass 35 and

37 on Faraday cup detectors with equivalent count rates of 2 to 5×107cps for 35Cl-. The measurements were made at sufficiently high mass resolution so as to eliminate all isobaric interferences, including 34SH- (Layne et al. 2004). We have developed two apatite standards for calibration: Durango apatite with a concentration of 0.37 wt. % Cl and a δ37Cl value of +0.33‰ 11 and a synthetic Cl-apatite from the University of Heidelberg with a Cl concentration of 5.5% and a δ37Cl value of +2.8‰. The δ37Cl values of these standards were previously determined by gas source mass spectrometry using the method described above. Precision of individual spot analyses ranged from 0.2‰ to 1.2‰ 1σSD depending on concentration of Cl in the apatite. External reproducibility is in the range of ≤0.5‰ for apatite with percent-level Cl concentrations like those of typical Martian meteorites (McCubbin et al., 2012, 2013, this issue).

3.0 Results

We collected bulk rock analyses of Cl isotopes and in situ Cl isotopic data from Cl-rich apatites in a wide range of martian meteorite petrologic types. Additionally, we divided the olivine-phyric shergottite Tissint into primary crystalline material and a glass component to determine the Cl- isotopic composition of each. The results from both bulk rock and apatite analyses are presented in Table 1 and 2 and illustrated in Figures 1 and 2. Bulk rock analyses of all the martian meteorites range from -3.9‰ to +1.8‰, and individual in situ apatite values range from -3.8‰ to +8.6‰. In the samples in which both bulk rock and apatite measurements were made, they were found to be nearly equal (Figure 1). For example, bulk rock analyses for Los Angeles and NWA 7034 are -

0.3‰ and +1.0‰, respectively, whereas individual apatite analyses range from -0.4‰ to -0.6‰ for Los Angeles and +0.1‰ to +8.6‰ (with an average of +1.2‰) for NWA 7034. Based on the agreement between apatite and bulk rock data in the instances where we collected both, we conclude that the in situ data and bulk rock data likely provide similar information, so we can proceed with discussing and grouping data for specific petrologic types when we have collected only in situ or bulk rock data as opposed to both.

δ37Cl (‰ vs SMOC) Cl (ppm) Petrologic Water Water type Sample SIMS Bulk Soluble Bulk Soluble

Olivine Phyric Shergottites Dhofar 019 -1.60 22 -0.60 RBT 04261 -3.50 - -2.50 -2.80 LAR 06319 -2.80 - -3.80 EETA 79001-A -2.65 180 Tissint Bulk -0.60 22 Tissint Glass -2.04 -0.43 69 136 Tissint Igneous -2.89 0.4 30 174 Basaltic Shergottites NWA 2975 0.10 24 Los Angeles -0.40 -0.30 -0.50 115 10 -0.60 Shergotty -3.30 108 Zagami -0.09 0.40 49 28 EETA 79001-B 0.22 42 Augite Basalt NWA 8159 1.5 - Nakhlites 13

NWA 5790 1.8 0.4 72 11 NWA 817 0.38 117 Chassignites NWA 2737 -3.85 Chassigny 0.4 - 0.3 Regolith Breccia NWA 7034 0.4 1 2200

0.4 0.4 0.5 0.5 0.5 0.5 0.6 0.6 0.7 0.7 0.7

0.9 1.1 1.1 1.4 1.5 0.1 8.6 14

Orthopyroxenite ALH 84001 1.4 -

Table 1: δ37Cl values and Cl concentrations of all Martian meteorites measured by bulk rock analysis and Secondary

Ion Mass Spectrometry Analysis.

Olivine Phyric Shergottites Basaltic Shergotitites Nakhlites Chassignites NWA 7034 ALH 84001 NWA 8159

Enstatite Chondrites

Ordinary Chondrites

Carbonaceous Chondrites The Moon CAI

Earth

-5 0 5 10 15 20 25 37 δ Cl

Figure 1: Cl isotope compositions of planetary bodies (Sharp et al. 2007, 2010a, 2010b, 2013, this issue). Symbols for bulk Earth are: brown= evaporites, white=halite inclusions from kimberlite, grey= carbonitite, black= MORB.

Averages are used for samples with multiple measurements expect for NWA 7034. 15

2 8.59‰, 4.79 wt% 1.8

1.6

1.4

1.2 Average Cl

37 1 δ 0.8

0.6

0.4

0.2

0 4 4.5 5 5.5 6 Cl (wt%)

Figure 2: In-situ measurements of apatite grains in all clasts analyzed from NWA 7034. Outlier point at δ37Cl =

8.59‰ not shown in figure. Error bars are 1σ.

Average δ37Cl

Grain Value Average Cl Content Clast type (number of spots) (standard (standard deviation)

deviation)

1B, 2 Grain 1 (4) 0.13 (0.07) ‰ 5.68 wt.% Mineral Fragment 16

1B,2 Grain 2 (1) 0.49 4.84 (0.20) FTP Clast 1

1B,2 Grain 3 (1) 0.73 5.08 Mineral Fragment

1B,2 Grain 4 (2) 0.70 (0.03) 5.11 (0.18) Mineral Fragment

1B,2 Grain 5 (1) 0.43 4.91 (0.05) Mineral Fragment

1B,2 Grain 6 (2) 8.59 (0.59) 4.79 Lithic Clast Fragment

3A,3 Grain 1 (2) 1.45 (0.10) 5.13 FTP Clast 12

3A,3 Grain 2 (1) 0.46 5.14 (0.04) FTP Clast 12

3A,3 Grain 3 (1) 0.60 5.14 FTP Clast 12

3A,3 Grain 4 (2) 0.44 (0.10) 4.69 (0.22) Lithic Clast Fragment

3A,3 Grain 5 (2) 0.73 (0.03) 5.08 (0.09) Mineral Fragment

3A,3 Grain 6 (1) 0.61 5.05 (0.13) Melt Clast

3A,3 Grain 7 (1) 0.37 5.31 Lithic Clast Fragment

3A,3 Grain 8 (2) 0.46 (0.09) 4.42 (0.18) Mineral Fragment

3A,3 Grain 9 (1) 0.87 5.01 (0.30) Mineral Fragment

2,3 Grain 1 (1) 1.36 4.78 Mineral Fragment

2,3 Grain 2 (1) 1.06 4.83 (0.05) Mineral Fragment

2,3 Grain 3 (2) 1.05 (0.29) 4.80 FTP clast

2,3 Grain 4 (2) 0.48 (0.10) 4.18 (1.07) Mineral Fragment

Table 2: Cl isotope ratios and Cl concentrations from apatite in basaltic breccia NWA 7034 determined from in situ measurements (Cl isotope ratios were measured using SIMS, and Cl concentrations were determined using EPMA).

Clast types follow Santos et al. (2015).

3.1 Overview of Cl isotopic results with petrologic types

When we grouped the meteorites based on their petrologic type, we observed several systematic trends with respective to Cl isotopic compositions among the various Martian meteorite lithologies, which are illustrated in Figure 1: (1) both LREE-enriched and depleted olivine-phyric shergottites Elephant Moraine 79001 lithology A, Roberts Massif 04261, Larkman Nunatak

06319, and Dhofar 019 have low δ37Cl values between -2.7‰ and -3.8‰ (Figure 1). The one exception to this range is the bulk rock value for LREE-depleted olivine-phyric shergottite Tissint, which yielded a bulk rock δ37Cl value of 0.6‰. This anomalously high value is investigated more closely in section 3.2. (2) The basaltic shergottites analyzed in this study are enriched (Los

Angeles, Shergotty, Zagami, NWA 2975) and intermediate (EETA 79001 lithology B) shergottites. They exhibit only minor variation in the δ37Cl values (-0.3 to +0.2) with the exception of Shergotty, which has a δ37Cl value of -3.3‰. The δ37Cl value of Shergotty is similar to the olivine-phyric shergottites (3) Other martian meteorites, exclusive of the shergottites such as the nakhlites, chassignites, regolith breccia NWA 7034, orthopyroxenite (ALH 84001), and augite basalt (NWA 8159), have positive 37Cl values (Figures 1 and 2), with the exception of chassignite

NWA 2737 (-3.85‰), which is similar to the light δ37Cl values exhibited by the olivine-phyric shergottites and Shergotty. Exclusive of NWA 2737, Chassigny and the nakhlites we analyzed exhibit δ37Cl values between 0.3‰ and 1.8‰ (Table 1). Although NWA 7034 has a bulk rock

δ37Cl value (1‰) similar to Chassigny and the nakhlites, the in situ analyses of apatite exhibit a large variation in δ37Cl values (+0.1‰ to +8.6‰), with an average δ37Cl value for apatite of 1.2‰.

The range in values in NWA 7034 apatites is likely linked to the different types of clasts incorporated into this sample, which appear to have originated from various types of crustal sources (Santos et al. 2015). The apatites within cumulate orthopyroxenite ALH 84001 have a 18

δ37Cl value of 1.4‰. We did not encounter any apatites in augite basalt NWA 8159, but we determined a bulk rock δ37Cl value of 1.5‰.

3.2 Cl-isotopic determination of primary and secondary components in Tissint

The olivine-phyric shergottite Tissint was a witnessed fall in 2011, and it represents our most recent martian meteorite fall with minimal terrestrial contamination (Aoudjehane et al.,

2012). Given the propensity for terrestrial contamination of Cl in meteorites with substantial terrestrial residence times, Tissint presented an opportunity to investigate both the water-soluble and insoluble Cl portions to gain insight into Martian Cl. Furthermore, Tissint is a highly shocked meteorite with numerous black glassy veins interpreted to be impact melt with trapped martian atmosphere based on excess 15N (Aoudjehane et al., 2012). Consequently, Tissint also provides the opportunity to investigate the Cl-isotopic composition of both the igneous and secondary impact components on Mars.

We did not encounter Cl-rich apatite in Tissint, so we only conducted bulk rock analyses of Cl isotopes. As indicated in section 3.1, the bulk rock measurement for Tissint is 0.6‰, which is higher than the range range exhibited by all of the other olivine-phyric shergottites (i.e., -2.7‰ and -3.8‰; Table 1). However, we also analyzed the Cl-isotopic composition of igneous

(crystalline) and impact glass (black glass) separates in Tissint, which exhibit minor, resolvable, variations in Cl isotopes for structurally bound Cl (-2.9‰ and -2.0‰ respectively) (Table 1, Figure

3). Given the low-degree of terrestrial contamination of Tissint, we also analyzed the water-soluble chlorine of the glass fraction and the igneous fraction, which had δ37Cl values of -0.4‰ and 0.4‰, respectively (Table 1). 19

Strucutral Water-Soluble Tissint Igneous Structural Water-Soluble 17% Tissint Glass 33% 7% 43%

Tissint Bulk Calculated Tissint Bulk

-3.5 -3.0 -2.5 -2.0 -1.5 -1.0 -0.5 0.0 0.5 1.0 37 δ Cl

Figure 3: δ37Cl value of all Tissint separates measured as well as the percent of the total Cl from each fraction.

4.0 Discussion

4.1 Comparison of Mars to variations of Cl isotopes in the Solar System

Over the last decade our group has determined the Cl isotopic compositions of numerous materials representing a variety of planetary environments including chondrites, the Moon, and the Earth (Figure 1). Mars provides a unique planetary environment to compare the nature and behavior of Cl isotopes. The differences are discussed in greater detail in our companion paper,

Sharp et al. (this issue). The bulk Earth has a δ37Cl value of 0‰ (Sharp et al. 2007). The Moon has a large variation in δ37Cl values, up to +35‰, but the undegassed, ‘primitive’ δ37Cl value is thought to be close to 0‰, similar to the Earth (Sharp et al. 2007; Shearer et al. 2014b; Tartèse et al. 2014;

McCubbin et al. 2015); however, there is an inexplicably light value of -4‰ recorded in apatite from lunar meteorite Miller Range (MIL) 05035 (Boyce et al., 2015). The averages of each chondrite class are indistinguishable from one another and overlap the bulk Earth value. These data were interpreted as evidence for a homogenous solar nebula with respect to Cl isotopes (Sharp et al. 2007, 2010a, 2013). 20

The bulk Martian meteorites and apatites have a much larger variation in δ37Cl values (-

3.85 to +8.6‰) than observed in deep-sourced rocks from the Earth, but not as broad as lunar samples (Figure 1). However, many of the mantle derived olivine-phyric shergottites, the chassignite NWA 2737, and Shergotty are distinctly isotopically light compared to the terrestrial mantle, most chondrites, and all lunar samples (sans MIL 05035). The negative δ37Cl values are difficult to explain in terms of known fractionation or mixing processes as discussed in the companion paper Sharp et al. (this issue). Although previous studies had reported that most chondrites, presumed to represent the solar nebula, have a δ37Cl value of ~0‰ (Sharp et al., 2007;

2013), Sharp et al. (this issue) point out that the samples studied previously had all been thermally altered to varying degrees and may not represent the primary Cl-isotopic composition of the solar nebula. Consequently, Sharp et al., (this issue) analyzed an unaltered 3.00 chondrite, NWA 8276

(a pairing with NWA 7731), which yielded a δ37Cl value of -4.5‰, similar to the chondrite

Parnallee (Sharp et al., 2013). Sharp et al. (this issue) interpret the values from NWA 8276 and

Parnallee as representative of the primitive solar nebula and posit that this primary nebula value has been recorded by a subset of the Martian meteorites analyzed in the present study.

Furthermore, it could explain the anomalously light δ37Cl value of -4‰ reported for apatite within lunar meteorite MIL 05035 (Boyce et al., 2015). Given that Mars is known to have accreted exceptionally fast compared to the other terrestrial planets (Dauphas and Pourmand, 2011), it could have recorded a primary nebular value within its interior during accretion, hence these light values are likely to represent the value of the Martian mantle.

The heavy Cl isotopic enrichments measured in Martian samples representative of the

Martian crust, such as apatite grains in NWA 7034 (regolith breccia), are unlike those observed at the Earth’s surface but similar in their 37Cl enrichment to soils and breccias from the Moon (Figure 21

1; Sharp et al., 2010a; Shearer et al., 2014b). Furthermore, they are similar to the heavy Cl-isotopic reservoir of the urKREEP component that is recorded in KREEP-rich basalts and highlands magnesian- and alkali-suite rocks (Boyce et al., 2015; McCubbin et al., 2015; Sharp et al., 2010a;

Shearer et al., 2015a).

4.2 Martian Mantle and Crustal Chlorine Reservoirs

Martian Crust

With respect to many geochemical parameters, the bulk composition of NWA 7034 mimics that of the bulk composition of the Martian crust as portrayed by the 2001 Mars Odyssey Gamma

Ray Spectroscopy (MOGRS) data (Agee et al., 2013; Keller et al. 2006; Boynton et al., 2007). The bulk composition of NWA 7034 also mimics many of the proposed geochemical and spectral characteristics of the Martian crust (e.g. Cannon et al., 2015; McLennan, 2001; McSween et al.

2009; Norman 1999; Taylor and McLennan, 2009). For example, REE patterns for NWA 7034 have similar slopes and concentrations to those predicted for the Martian crust (Nyquist et al.,

2016). Further, this sample has recently been shown to contain the first Martian sedimentary clast

(McCubbin et al., 2016b; Wittmann et al., 2015). The high Cl concentration of 2200 ppm for NWA

7034 is the highest measured in any Martian sample, but still at the lower end of the Cl concentration range of the surface of Mars (Agee et al., 2013; Shearer et al., 2014a). Based on the presence of crustal materials and the chemical similarities to bulk martian crust, we find it appropriate to use the isotopic composition of this sample as representative of the martian crust.

The δ37Cl values determined by in-situ analysis of NWA 7034 apatites indicate that the

Martian crust is enriched in heavy Cl relative to the Martian mantle, which will be discussed later in detail. The variability in this enrichment (δ37Cl = 0.1 to 8.6 ‰) could indicate differences in the 22 amount of crustal Cl assimilated in various clasts, or more likely, that the crust of Mars is heterogeneously enriched in the heavy isotope of Cl. Figure 2 plots all in-situ measurements of

δ37Cl values vs. measured Cl concentrations. The majority of apatites in this breccia have a narrow range of Cl isotopic compositions and concentrations. One clast, 1B,2 Grain 6 (lithic clast fragment), has an apatite with a δ37Cl of 8.60 ‰ and a concentration of 4.79 wt% Cl. This suggests that the Martian crust was highly isotopically fractionated, relative to the mantle, since at least 1.5-

1.7 Ga ((Bellucci et al., 2015; Cartwright et al., 2014; McCubbin et al., 2016b). The 1.5-1.7 Ga ages are for U-Pb in apatite, metamict zircon, and bulk rock K-Ar, which has been interpreted as the age of breccia lithification originating from a thermal event (Bellucci et al., 2015; Cartwright et al., 2014; Humayun et al., 2013; McCubbin et al., 2016b; Muttik et al., 2014). The igneous components in NWA 7034 are older, up to 4.4 Ga (Humayun et al., 2013; McCubbin et al., 2016b;

Nemchin et al., 2014; Nyquist et al., 2016).

The process that caused the heavy δ37Cl value of the crust could be related to the same mechanism responsible for the heavy isotopic composition of Martian atmophile elements, which would imply interaction between the Martian atmosphere and crust. Mars has lost a significant portion of its atmosphere through billions of years of interaction with solar wind (Chassefière and

Leblanc, 2004). Mars is susceptible to this loss in absence of a magnetosphere. This interaction effectively strips the atmosphere and causes large mass-dependent fractionation by preferential loss of the light isotope to space. D/H, 15N/14N and 38Ar/36Ar show large enrichments in the heavy isotope partly attributed to this sputtering reaction (e.g. Owen et al. 1977; Becker and Pepin 1984;

Mathew and Marti 2001). Chlorine is likely concentrated in the Martian crust and atmosphere through volcanic degassing of HCl. HCl gas could also be produced by low-temperature fluid-rock interaction. Jarosite has been identified by the Mars Exploration Rover (MER) Opportunity 23

(Klingelhofer et al., 2004) and within Martian meteorites (McCubbin et al. 2009). This is strong evidence that the hydrosphere of Mars may have been acidic, at least locally. If an acidic fluid interacts with NaCl it can volatilize Cl through the following reaction: NaCl (s) + H2SO4 -> HCl

(g) + NaHSO4 (aq). Perchlorate formation has also been shown to produce a significant volatile species of Cl (Hecht et al. 2009). Preferential loss of H35Cl relative to H37Cl to space through time would cause a large positive shift in the δ37Cl of the atmosphere and ultimately, the crustal reservoir, leaving a isotopically light mantle reservoir (37Cl = ~ -3 to -4‰) and a isotopically heavy crustal reservoir (37Cl ≥ 1‰). As a first order analog, Argon shows similar heavy isotope enrichment for the same overall molecular mass, so there can be little doubt that HCl gas is able to escape Martian gravity.

Additional evidence for the heavy Cl isotopic signature being related to a surface- atmospheric component is its correlation to the sulfur isotopic composition of Martian meteorites.

Sulfur is an ideal system for tracking the incorporation of material that has been at the surface of

Mars. There are four stable isotopes of sulfur (32S, 33S, 34S, and 36S). Mass independent fractionation for sulfur occurs during photochemical reactions (Thiemens, 1999) and has been documented for a number of reactions involving sulfur isotopes (Farquhar et al., 2000, 2001). The most significant source of sulfur mass-independent fractionation (S-MIF) is gas phase photochemistry driven by ultraviolet (UV) radiation (Cooper et al., 1997; Farquhar et al., 2001;

Rai et al., 2005; Rai and Thiemens, 2007). The resulting sulfur species, characterized by an anomalous isotopic composition due to this fractionation, may subsequently transfer this fingerprint from the atmosphere to solid phases. This effect, which results in Δ33S and Δ36S values that do not lie on a predicted mass-dependent array, has been documented in terrestrial sedimentary deposits and in some meteorites (Cooper et al., 1997; Farquhar et al., 2001; Rai et al., 2005; Rai 24 and Thiemens, 2007). Franz et al. (2014) reported on the Δ33S anomalies in some Martian meteorites. Franz et al. (2014) interpreted these observations as evidence for cycling of sulfur between an atmospheric reservoir where photochemical processing of sulfur-bearing gases occurred and a surface reservoir in which photochemical products were ultimately deposited. The incorporation of these S-MIF fingerprints into products of Martian magmatism implies mixing of sulfur from the Martian surface into the basalts through assimilation by lavas/magmas or interaction with crustal fluids.

A plot of δ37Cl versus Δ33S (Figure 4) shows that the olivine phyric shergottites with δ37Cl values of less than -3‰ (RBT 04261and LAR06319) and basaltic shergottite Shergotty do not have a Δ33S anomaly. All samples with more positive δ37Cl values also have a Δ33S anomaly, which is consistent with our hypothesis that positive δ37Cl values are indicative of crustal assimilation. This correlation suggests that use of these isotopic systems tangentially distinguishes between the primitive isotopic composition of the mantle and the crust. It further suggests that the crustal signature is characteristic of the crust for at least 1.5-1.7 billion years and, if based solely on Cl, perhaps as long as 4.1 billion years. ALH 84001 is the oldest unbrecciated sample measured with an age of 4.09 Ga (Lapen et al. 2010). Even if the metamorphic age of ALH 84001 (3.9 Ga;

Borg et al., 1999) is used as the constraint for the timing of δ37Cl incorporation, the results imply the previously mentioned crustal chlorine fractionation occurred within the first 500Ma of Mars history. 25

0.1 Olivine Phyric Shergottites

0.08 Basaltic Shergottites Chassignites 0.06

S 0.04 33 Δ 0.02

0 Sulfur Mass-Dependant Fractionation Line

-0.02

-0.04 -4.00 -3.00 -2.00 -1.00 0.00 1.00 δ37Cl

Figure 4: Plot of Δ33S vs. δ37Cl. The sulfur mass dependant fractionation line is defined by equations in Farquhar et al. (2000, 2001). Sulfur data is from Franz et al. (2014). Error bars are 1σ. Averages are used for samples with multiple measurements.

Taylor et al. (2010) suggested that bulk Mars has a chondritic Cl/K ratio based on the average of orbital data from the 2001 Mars Odyssey Gamma Ray Spectrometer. However, this ratio is relatively heterogeneous and can be geographically isolated (Taylor et al. 2010). Our suggestion that the Cl isotopic composition of the crust is representative of fractionation though mass dependent dynamic escape suggests that the bulk Martian crust should have a sub-chondritic

Cl/K if a significant proportion of Cl was lost to space. A first order calculation assuming Grahams

law diffusion (� = ) with the Raleigh fractionation equation suggests approximately 26

36% of the crustal Cl would have to be lost to change the chlorine isotopic composition by 12‰; although if the crustal value is representative of the bulk rock value of the regolith breccia (i.e.,

1‰; Table 1), it would still imply a loss of approximately 14% crustal chlorine. These calculations imply that Mars had an initial super-chondritic Cl/K because the surface is presently near chondritic (Taylor et al., 2010). Another possibility is that the Cl/K observed on the Martian surface has been influenced by degassing of Cl and hydrothermal activity that would raise the apparent Cl/K on the surface relative to its source due to the hydrophilic nature of Cl compared to

Martian Mantle

The olivine-phyric shergottites, including Yamato 980459 and ALH77005 (intermediate lherzolite), are thought to represent our closest approximations of crystallization products of primary Martian basalts. Both the olivine-phyric shergottites and basaltic shergottites exhibit an enormous range in several isotopic and geochemical signatures compared to Earth. For example, a prominent geochemical feature of the shergottites is the large range in initial Sr isotopic ratios and initial εNd values (Shih et al. 1982, 2003, 2004, 2005; Nyquist et al. 1979, 2000, 2001, 2006;

Borg et al. 1997, 2001, 2003, 2005, 2012; Brandon et al. 2004, 2012; Symes et al. 2008; Shearer et al. 2005, 2006, 2008). This range far exceeds the range observed in all terrestrial mantle derived basalts (Borg et al. 2005, 2012). Within this range, the shergottites do not form a radiogenic isotopic continuum, but instead, they fall into three discreet subgroups. These subgroups have distinct characteristics such as the bulk rock REE patterns, mineral chemistries (i.e. phosphate

REE patterns, Ni, Co, V in olivine), and oxygen fugacity during crystallization (Herd et al. 2002;

Herd, 2003, 2006; Wadhwa 2001; Borg and Drake, 2005; Borg et al. 2003, 2005; Shearer et al.

2006, 2008, 2015b; Symes et al. 2008). 27

Although there are significant geochemical differences among the depleted (Tissint), intermediate (Elephant Moraine 79001 lithology A), and enriched (Roberts Massif 04261,

Larkman Nunatak 06319, Dhofar 019) olivine-phyric shergottites, these samples all have low δ37Cl values, ranging from -3.8‰ to -2.04‰. As Cl does not fractionate during high temperature processes such as fractional crystallization and partial melting (i.e., Sharp et al., 2007; Sharp and

Draper, 2013), and because these samples have no direct petrographic evidence for fluid alteration, our interpretation is that these light Cl isotope values are representative of the Martian mantle (see

Sharp et al., this issue). This conclusion is further supported by the S isotopic composition of these basalts. As noted earlier, the Δ33S of these samples are 0‰ (Franz et al. 2014) indicating that they have not interacted with S derived from crustal-atmosphere interactions at the Martian surface

(Figure 4).

Dhofar 019 has a slightly higher δ37Cl value than other olivine phyric shergottites, δ37Cl =

-1.6‰. However, this higher value can be attributable to secondary processes. Dhofar 019 displays strong evidence for secondary alteration including the formation of calcite and gypsum, and it exhibits extreme enrichment of Sr (Folk et al. 2001). It has been suggested that this alteration is terrestrial, as this meteorite was a find in the Oman dessert (Folk et al. 2001). However, Taylor et al. (2002) have also suggested that this alteration may have formed on the surface of Mars. It is unclear whether or not the chlorine isotopic composition of Dhofar 019 is reflective of terrestrial or Martian weathering, but it is probably not reflective of the primitive Martian mantle.

Both Shergotty (basaltic shergottite) and NWA 2737 (chassignite) exhibit light Cl isotopic compositions (Table 1), similar to the olivine-phyric shergottites, indicating that they may record a Cl isotopic signature from the same source as the olivine-phyric shergottites, which we attribute to a mantle signature. Shergotty is petrologically similar to the enriched basaltic shergottites 28

Zagami and Los Angeles, and all three are geochemically enriched and relatively oxidized, but

Shergotty contrasts strongly with Zagami and Los Angeles in Cl isotopes (Table 1). The mantle- like δ37Cl value for Shergotty corresponds to a Δ33S value of 0‰, which supports the interpretation that the Cl isotopic composition of Shergotty represents a mantle signature. In contrast, Zagami and Los Angeles both have isotopically heavy δ37Cl values and both exhibit positive Δ33S anomalies (Table 1; Franz et al., 2014). NWA 2737 is a cumulate igneous rock that records extensive secondary shock effects that have disrupted noble gas systematics (Marty et al., 2006) as well as D/H systematics (e.g., Giesting et al., 2015), which renders questionable a mantle interpretation for the δ37Cl value of NWA 2737. However, loss of Cl through volatilization of HCl or metal chlorides typically does not affect or drives to higher values the initial δ37Cl value of a sample (Sharp et al., 2010a,b; McCubbin et al., 2015), so we do not attribute the low mantle-like

δ37Cl value of NWA 2737 (-3.85‰, Table 1) to secondary shock effects and support the interpretation of a mantle signature.

Studies of radiogenic isotopic systems such as Sm-Nd and Rb-Sr have shown that the

Martian mantle is heterogeneous and that the martian meteorites sample at least two mantle reservoirs and perhaps more (Sarbadhikari et al., 2009, 2011; Shih et al. 1982, 2003, 2004, 2005;

Nyquist et al. 1979, 2000, 2001, 2006; Borg et al. 1997, 2001, 2003, 2005, 2012; Brandon et al.

2004, 2012; Symes et al. 2008; Shearer et al. 2005, 2006, 2008). Figure 5 further demonstrates how the Cl isotopic compositions of martian meteorites relate to geochemical enrichment indicated by ε143Nd values. Figure 5 illustrates that isotopically light Cl values in the range of -2.8‰ to -4‰ are recorded in martian meteorites that span geochemically enriched, intermediate, and depleted sources. If our interpretation that the primitive Martian mantle is homogenously light with respect to Cl isotopes, deviations from a mantle Cl isotopic value likely result from secondary mixing with 29 heavier components like the Martian crust. Furthermore, our interpretation supports the idea that there are geochemically depleted, intermediate, and enriched reservoirs in the martian mantle, and

Cl isotopes could be utilized as a tracer for crustal contamination in martian meteorites.

45.00

35.00

25.00

15.00 Nd

143 5.00 Olivine Phyric Shergottites ε Basaltic Shergottites -5.00 Nahklites Chassignites -15.00 -4.00 -3.00 -2.00 -1.00 0.00 1.00 2.00 3.00 37 δ Cl

Figure 5: Plot of δ37Cl vs. ε143Nd demonstrating that across the isotopically different reservoirs, the Martian mantle has low chlorine isotope ratios. There is no difference between enriched and depleted shergottites. Nd data taken from

Jagoutz and Wänke, (1986); Borg et al. (2001); Nyquist et al. (2001); McCubbin et al. (2013). Averages are used for samples with multiple measurements.

The homogeneity of the Martian mantle with regards to Cl isotopes and the heavy Cl isotope composition of the Martian crust have profound implications for petrogenetic models for

Martian magmatism. Many of the REE and isotopic characteristics of the shergottites have been linked to different reservoirs in the crust and mantle and their interactions during the petrogenesis of shergottite magmatism. Two end-member petrogenetic models have been suggested to account for the location and interaction of these reservoirs and the variation in shergottite compositions.

All of these reservoirs seem to have formed within the first 30-50 Myr of the formation of the 30

Solar System (Borg and Draper, 2003, Bouvier et al. 2009). In one model, the shergottite compositional array is a product of melting (and mixing) of two distinctly different mantle sources; a reduced (IW-1 to IW+1), depleted mantle and enriched mantle that is either oxidized or its melting products have undergone secondary oxidation during or prior to crystallization (Blinova and Herd 2009; Papike et al. 2009; Shearer et al., 2013). An alternative model is that the shergottites that are reduced and depleted reflect the Martian mantle, whereas the more oxidized and enriched shergottites indicate interaction between mantle-derived basalts and the Martian crust. To distinguish between these two models, a fuller understanding of the petrologic linkages among all of these geochemical characteristics and intensive parameters (fO2) must be reached.

One approach to deciphering these petrogenetic linkages is unraveling the crystallization history preserved in olivine megacrysts in the more primitive shergottites (olivine-phyric shergottites).

The isotopically light δ37Cl values of both the enriched and depleted mantle sources indicate that the formation of these reservoirs is not a product of mixing of a crustal component. The nature of mixing of the two Cl isotope reservoirs will be examined in the next section.

4.3 Mechanisms of Mantle-Crust Interactions

Placing the Cl isotope signatures of the Martian meteorites into the context of their textures, mineralogy, and geochemistry provides evidence for a variety of mechanisms for interactions between mantle-derived magmas and the Martian crust. These mechanisms include mechanical mixing during impact and other surface processes, interactions between crystallized basalts and crustal fluids, and assimilation of the crust by mantle-derived basaltic melts. Here, we give examples of each process and consider the relative likelihood of each in reproducing the observed changes in Cl isotopic composition. 31

Assimilation and fractional crystallization (AFC)

The importance of crustal assimilation for the generation of shergottites is unsettled (see

Shearer et al., 2013; Papike et al. 2009). We can address the degree of assimilation using the isotopes of Cl, S, and Li because the crustal and mantle end member values are so different. These light element isotopic systems may be more sensitive than REE systematics in tracing low degrees of crustal assimilation.

The chlorine concentration in olivine phyric shergottites ranges from 20 to 50 ppm but the concentration in the crust has been shown to be significantly higher and variable, between 2000 ppm and 1 wt% (Wänke and Dreibus, 1994; Keller et al. 2006; Taylor et al. 2010; Bogard et al.

2010; McCubbin et al., this issue). It is also likely that the isotopic composition of the crust is highly variable as discussed earlier. As shown in Sharp et al. (this issue), a simple mixing model indicates that all of the measured Cl isotopic compositions of the basaltic shergottites (other than

Shergotty, which exhibits anomalously light Cl values) can be explained by an addition of less than 2% crustal assimilant.

Assimilation of crustal material would also have important implication for other elemental systems. To assess this effect, Figure 6 shows an assimilation fractional crystallization (AFC) model for varying degrees of assimilation. The two dashed lines represent a simple mixing model of Cl isotopes and the La/Sm ratio from both the LREE depleted (Yamato 980459) and LREE enriched (Roberts Massif 04261) mantle reservoirs with a highly LREE enriched Martian crust

(Taylor and McLennan. 2009). The grey lines track the change in the La/Sm as olivine crystallizes; we assume that this process does not effect the δ37Cl values. Appropriate partition coefficients

(from McKenzie and O'Nions 1991) were chosen under the assumption that only olivine would be 32 removed from the system. It is important to note that AFC from the LREE depleted reservoir does not appear to explain the LREE enriched shergottites and therefore evolution from a previously enriched reservoir is required to explain their chemistry.

The low degrees of AFC indicated by the δ37Cl values has little effect on the REE patterns, which clearly demonstrates the insensitivity of REE to low degrees of crustal assimilation. For example, the sample Shergotty (enriched shergottite) is largely indistinguishable from Los Angeles

(enriched shergottite) in REE space (Figure 6). Los Angeles is only slightly more enriched with respect to REE patterns. However, the Cl isotope composition of these samples shows a significant difference (Figure 6). Shergotty appears to be representative of an unaltered mantle derived basalt, and Los Angeles has been affected by a Cl-rich, isotopically heavy, crustal assimilant.

30% NWA 8159 10% 10% Martian Crust

5% 5%

EETA 79001-B NWA 2975 2% 2% La Lu Zagami Los Angeles

Tissint (Bulk) 1% 1%

DHO 019

odel odel

M M

ixing ixing

M Y98 M RBT 04262

EETA79001-A

Shergotty

RBT 04262 La Lu La Lu LAR 06319

Figure 6: Assimilation fractional crystallization model (black line) and mixing model (dashed black lines) showing interaction effects from depleted and enriched Martian reservoirs with an estimated Martian crustal composition

(Taylor et al. 2010). Values next to model lines represent the amount of assimilated material. Partition coefficients used assume olivine is removed from the system (McKenzie and O'Nions 1991). Averages are used for samples with multiple measurements.

This AFC model provides valuable insights into martian geochemistry and petrology. It demonstrates the usefulness of Cl isotopes as a sensitive indicator for crustal assimilation where other elemental systems, such as REE, fail to elucidate these interactions. More importantly, Cl- isotopes reveal a new window into differentiating between samples that are representative of geochemically enriched mantle vs samples that have been contaminated by enriched crust on Mars.

Cl-isotopes has the potential to become an important petrogenetic discriminator on Mars, especially in combination with REE geochemistry, estimates of oxygen fugacity, and other stable isotopic systems, including S and Li.

Mechanical mixing

Several Martian meteorites consist of an igneous component and pods, pockets, and/or veins of impact-derived glass materials (e.g. EETA 79001 lithologies A, B, and C; Tissint). In

Tissint, the bulk composition of the impact glass appears to be a mixture of the igneous component and a soil and/or crustal component (Aoudjehane et al. 2012; Magna et al. 2015). Tissint igneous and impact glass separates show minor, resolvable, variations in δ37Cl of structurally bound Cl (-

2.9‰ and -2.0‰ respectively) (Table1, Figure 3). Compared to the bulk measurement for Tissint of -0.6‰ in Table 1, a third component is required for mass balance. This third component is the water-soluble chlorine of the glass fraction, with a measured δCl value of -0.4‰. This fraction contains 33% of the total Cl. This component most likely represents the influence of weathering 34 near the surface of Mars that has been documented by Aoudjehane et al. (2012). The impact glass found throughout Tissint makes up approximately 20% of the meteorite. A mass balance of all fractions analyzed yields a δ37Cl of -0.5‰ per mil, identical within error to the previous bulk measurement of -0.6‰ (see Table 1, Figure 3). Therefore, this agreement supports the idea that the glass found in Tissint may source a crustal, potentially soil-like, material (Aoudjehane et al.

2012). Furthermore, this result indicates how impact processes may potentially alter primary Cl- isotopic signatures of a sample through mechanical mixing processes.

Fluid interaction

It has been long recognized that low-temperature mineral assemblages of Martian origin are preserved in some Martian meteorites. These assemblages are largely interpreted as alteration products from Martian fluids and brines. They include Fe-rich smectite, serpentine, fluid inclusions, and amorphous gels among others and are generally found along veins (Bridges and

Grady, 2000; Changela and Bridges, 2010; Bridges and Schwenzer, 2012; Hallis et al. 2014).

In addition to low-temperature alteration, the Martian meteorites also exhibit evidence of high-temperature hydrothermal activity and magma-fluid interaction. The most well-documented evidence for high-temperature hydrothermal activity has been with the chassignites and nakhlites.

The nakhlites and chassignites are generally interpreted as comprising a cumulate igneous pile

(Day et al. 2006; Hallis and Taylor 2011; Harvey and McSween, 1992; Imae et al. 2005; Lentz et al. 1999; Mikouchi et al. 2003, 2012; Treiman 2005; Treiman and Irving 2008), and they have recently been proposed to be of co-magmatic origin (McCubbin et al. 2013). The chassignites are dunites consisting of cumulus olivine and chromite and are thought to be at the base of this cumulate pile. The nakhlites are clinopyroxenites with cumulus clinopyroxene and olivine grains, 35 thought to be stratigraphically higher than the chassignites (Floran et al. 1978; Treiman 2005; Beck et al. 2006; Mikouchi et al. 2012; McCubbin et al 2013). Both meteorite groups are very Cl-rich with respect to other Martian meteorites and show evidence for aqueous/hydrothermal alteration by Cl-rich fluids/brines (Bridges and Schwenzer, 2012; Filiberto et al., 2014; McCubbin and

Nekvasil, 2008; McCubbin et al. 2009, 2013).

The δ37Cl values of both nakhlites (NWA 5790 and NWA 817) and matrix apatites (i.e. not found in melt inclusions in olivine) in Chassigny have positive δ37Cl values. This suggests that a Cl-rich brine of crustal origin interacted with these samples, which is consistent with previous models proposed for the Chassigny meteorite (McCubbin and Nekvasil, 2008). The range in Cl isotope compositions seen in these samples may give an indication as to the degree of fluid interaction, where NWA 5790 has exchanged most with the crustal fluid. One interesting difference is seen in the two measured chassignites, NWA 2737 and Chassigny. The matrix apatites measured in

Chassigny have δ37Cl values between 0.3 and 0.4‰ but the bulk rock measurement from NWA

2737 has a δ37Cl value of -3.85‰. It has been observed that NWA 2737 experienced a lesser degree of Cl-enrichment in apatite than Chassigny (McCubbin et al. 2013). The Cl isotopic composition of NWA 2737 further supports this idea as it has retained a mantle-like Cl signature despite the apparent shock effects and isotopic resetting seen in other systems (Beck et al., 2006; Marty et al.,

2006; Treiman et al., 2007; Pieters et al., 2008; He et al., 2013; Giesting et al., 2015). Chassigny, on the other hand, appears to have exchanged with a crustal fluid to some extent at least within the portions of the meteorite that are interstitial to the cumulus olivine grains.

7 Olivine Phyric Shergottites Basaltic Shergottites Chassignites 6 NWA 7034 ALH 84001 Nahklites 5

37 δ Clcrust=8.00‰ 4 Li

7 3 Martian Mantle δ

-1 -4.00 -3.00 -2.00 -1.00 0.00 1.00 2.00 3.00 4.00 37 δ Cl

Figure 7: Plot of δ7Li vs. δ37Cl (Magna et al. 2015). Model lines are simple mixing models as discussed in text.

Error bars are 1σ. δ7Li value for Dhofar 019 taken from Reynolds et al. (2006). Averages are used for samples with multiple measurements.

The noble-gas composition of Chassigny is representative of the Martian mantle and has not exchanged with a crustal or atmospheric reservoir (Mathew and Marti, 2001; Mathew et al.

1998). Therefore, it might be expected that the Cl isotopic composition would also support the same conclusion. In fact, McCubbin and Nekvasil, (2008) reported that apatites within olivine- hosted melt inclusions in Chassigny are depleted in Cl relative to the intercumulus apatites. We hypothesize that the Cl isotopic composition reflected in the matrix apatites indicates fluid 37 exchange and alteration but that the fluorine-rich apatites hosted in melt inclusions may reflect an unaltered mantle derived δ37Cl value, which is reflected in the noble gas composition of the cumulus olivines, although additional analyses of apatites from the olivine-hosted melt inclusions in Chassigny are required to test this hypothesis.

Lithium has been used in many systems to track fluid interactions and low temperature alteration (e.g., in MORB; Elliot et al. 2006; Tomascak et al. 2008). Li isotope fractionation has been shown to occur in low-temperature processes. During weathering and fluid interaction, secondary phases preferentially incorporate the light isotope, leaving a heavy residue (Magna et al. 2015; Pistiner and Henderson, 2003; Rudnick et al., 2004; Vigier et al., 2008; Wimpenny et al.,

2010). Magna et al. (2015) showed that Li isotopes in Martian meteorites have a large variation

(+5.0 to -0.2‰). The Bulk Silicate Mars, as represented by the olivine-phyric shergottites and other unweathered samples, has a δ7Li value of +4.2‰, but the Martian crustal Li isotopic composition has a much lighter value, potentially reflected by NWA 7034 of -0.2‰. Figure 7 displays the Li isotopic compositions against the Cl isotopic compositions as shown by Magna et al. (2015). Figure 7 shows a general negative correlation with a much tighter clustering around the primitive Martian mantle signatures of both isotopic systems: δ7Li of 4.2‰ and δ37Cl value of -

3.8‰. Mixing curves between mantle and crust for these two isotope systems were calculated for three different assumed 37Cl values of crust; all other parameters were kept constant: 1) Mantle

-- δ7Li = +4.2‰, Li conc. = 2 ppm (Magna et al., 2015), 37Cl = -4‰, Cl conc. = 20 ppm; Crust

-- δ7Li = -0.21‰, Li conc. = 12 ppm,37Cl = 0‰, +2‰, and +8‰ (three separate curves), Cl conc. = 2000 ppm. Li isotope composition and concentrations have little effect in these models due to the much narrower difference in the concentrations and isotopic compositions of the mantle and crustal reservoirs compared to Cl. The mantle concentration of Li is near 2 ppm, indicated by 38 the meteorite record (Magna et al. 2015), in contrast, the crust has been suggested to have a concentration of around 10 ppm as measured by the Mars Science Laboratory (MSL) rover

Curiosity and the meteorite record (Magna et al. 2015; McLennan et al., 2014; Ollila et al., 2014).

As a consequence, only the Cl isotope composition of the Martian crust was varied in these models.

All samples, with the exception of Dhofar 019, fall into the array defined by 37Cl crustal values between 0 and 8‰. This is a further indication that the crustal Cl-isotopic reservoir is highly variable and may be spatially dependent.

5.0 Conclusion

Our study found that Mars has at least two isotopically distinct chlorine reservoirs, the mantle and the crust. The δ37Cl value of the Martian mantle, as represented by the olivine-phyric shergottites, NWA 2737, and Shergotty, is lighter than all other known planetary bodies with a

δ37Cl value of approximately -3.8‰. The δ37Cl value of the Martian crust is reflective of a highly isotopically fractionated atmosphere and is potentially heterogeneously enriched in the heavy isotope of Cl. Due to the large concentration difference of Cl in the mantle and crust, the Cl isotope system acts as a sensitive recorder of crust-mantle interaction. It appears that the petrologic linkages among the SNC meteorite reservoirs cannot be explained solely by assimilation of crustal material, as all mantle reservoirs (depleted, intermediate, and enriched) are homogenous with respect to Cl isotopes, despite variations in Sm-Nd and Rb-Sr isotopic systematics as well as LREE enrichment. This observation further supports the idea that there are geochemically enriched reservoirs within the Martian mantle. Assimilation of crustal material into these reservoirs would have caused a positive shift in the δ37Cl values. The meteorite record contains samples that lie upon a continuum of exchange with the Martian crust after extraction from mantle reservoirs. The 39 nature of this interaction can be mechanical, fluid/brine interaction, and assimilation fractional crystallization.

6.0 Acknowledgements

This work was supported by NASA under award # NNX14AG44G to Sharp and Shearer and a

Humboldt Fellowship to Sharp. The UCLA ion microprobe laboratory is partially supported by a grant from the NSF Instrumentation and Facilities Program. FMM acknowledges support from the

NASA Mars Fundamental Research Program during this study through grant NNX13AG44G awarded to FMM.

CHAPTER 2

Tracking Cl in Primitive Ordinary Chondrites:

Evidence for HCl-Clatherate Formation in the Solar Nebula

J.T. Williams1,2, Jon Lewis1, Z.D. Sharp1,2, A.J. Brearly1. S.A. Singerling1

1Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, NM,

87131, USA, [email protected]

2Center for Stable Isotopes, University of New Mexico, Albuquerque, NM, 87131, USA

Abstract

The study of volatile elements and their incorporation into planetary bodies is closely tied and fundamentally important to our understanding of the environmental conditions of the solar nebula.

The processes through which volatile elements, such as the halogens, are incorporated into chondritic parent bodies are still very much debated. Cl can be employed effectively in the study of this issue, as it is immensely useful both as a cosmochemical and geochemical tracer in chondrites due to its volatile, hydrophilic and incompatible characteristics. The average chlorine isotope composition of chondrites is similar to Earth’s – close to 0‰ – though there is a 3‰ overall spread. In contrast, NWA 8276, a primitive 3.00 LL chondrite, has an isotopically-light Cl value of -4.5‰ that has previously been attributed to inheritance of the primitive δ37Cl of the solar nebula. This work presents the Cl isotopic composition of all other known 3.00 ordinary chondrites, NWA 7731, NWA 10061 and Semarkona. Unlike NWA 8276, these samples all have

Earth-like δ37Cl values. The explanation for this difference is elucidated through the petrographic study of NWA 8276, NWA 10061 and Semarkona. Semarkona displays petrographic evidence for

Cl incorporation into chondrules prior to parent body accretion. This incorporation is attributed to the formation of an HCl-clathrate, which is predicted to be isotopically-heavier than nebular gas – on the order of 3-6‰. We demonstrate that these chondrules in Semarkona were altered by a Cl- bearing fluid consistent with clathrate formation. NWA 10061 was also found to contain areas that are both rich in Cl and consistent with the clathrate model. In contrast, NWA 8276 only contains

Cl in the matrix. We interpret this Cl to be nebular in nature, perhaps sourced from the condensation of NaCl or sodalite during nebular cooling. NWA 8276 appears to have escaped the 42 incorporation of HCl-clatherate ice, and therefore preserves the primitive Cl isotopic composition of the solar nebula.

1.0 Introduction

Chondritic meteorites represent the earliest rocks formed in our solar system, spanning a broad range of chemical compositions and histories. They consist of 4 major components: Chondrules;

Calcium-Aluminum Inclusions (CAI’s); metal; and matrix. These components vary in size and abundance between classes. Chondrules are largely thought to be igneous melt droplets formed in the early nebula that crystallized with differing cooling-rates and chemistries (Scott and Krot,

2004). It is unlikely that many volatile elements were originally incorporated due to the high temperature of the initial chondrule formation. This is evidenced by the lack of primary, halogen- bearing phases found in chondrites and their components (Brearly and Jones, in prep). Chondrules were accreted with smaller fragments of material, nebular dust and metal to form a primitive chondrite. After this initial state, the bodies experienced different degrees of thermal and aqueous alteration. Using standardized techniques, the different chondritic meteorites are categorized according to class (e.g. OC, CI, CV, etc.), thermal metamorphic grade on a scale of 3.00 to 6, and aqueous alteration grade on a scale of 1 to 3.00 (Grossman and Brearley 2004; Huss et al., 2006).

A metamorphic grade of 3.00 represents the most pristine samples, signifying minimal alteration.

Chondritic meteorites are thought to be the closest representation of the building materials for the inner planets. As such, understanding how volatile elements are incorporated into chondrites is of paramount importance in the identification of similar volatile sources comprising the terrestrial planets. 43

It has long been debated how volatile and moderately-volatile elements are incorporated into chondritic asteroids (e.g. Brearly and Jones, in prep). Further, many of these elements are easily mobilized during aqueous and thermal alteration events, which erases the chemical and textural evidence of their original incorporation. The halogens (F, Cl, Br, and I) are volatile elements of particular cosmochemical significance. It should be noted that Cl has been classified as both a moderately-volatile element (Lodders 2003) and as a volatile element (Palme and Jones 2003).

The discrepancy is due to a lack of primary-condensation phase-identification that incorporates

Cl. This study will refer to Cl as a volatile element, as explained in greater detail in the following sections. The halogens are found in varying concentrations across the identified chondrite groups without chemical or alteration correlations. The highest Cl concentrations are found in the strongly aqueously-altered CI chondrites (Brearly and Jones, in prep).

Cl is both strongly hydrophilic and incompatible in magmatic systems (Sharp and Draper

2013). Together with fluorine, chlorine is found in high concentration in chondrites (100s of ppm) and is therefore useful as an attainable geochemical proxy for many systems. All Cl-bearing phases found in chondrites are identified as secondary minerals and include chlorapatite, sodalite, and smectite (e.g. Brearley and Krot 2013 Brearly and Jones 2016, Sharp et al., 2007,2013). Often these phases are found in the chondrule mesostasis and in the matrix of chondrites. This has led to the prevailing idea that Cl – along with the other halogens – is largely brought in through aqueous processes on the parent body post-accretion (see Brearly and Jones, in prep).

As with many elemental systems, isotopic analysis can be used to elucidate the difference in origin and histories among samples. The Cl-isotope compositions of many chondrite groups have been measured by Sharp et al., 2007, 2013. These studies found isotopic compositions (δ37Cl) ranging from -2‰ to +1.2‰ (Figure 1). Only one sample, Parnallee (LL3.6), was found to be an 44 outlier at δ37Cl=-4.2‰ (Figure 1). The average of all chondrite groups was approximately +0.3‰, within error of the Earth’s bulk Cl isotopic composition. These studies concluded that the initial solar nebula had a δ37Cl of 0‰ (relative to standard mean ocean Chloride). The variations from this initial value were attributed to local parent body fractionations after incorporation. These mechanisms included pore-fluid migration and, in the case of Parnallee, incorporation of a light

HCl-gas after formation of a HCl-clathrate in the nebula, as suggested by Zolotov and Mironenko

2007. Further, there appeared to be little correlation between isotopic composition and chondrite group, petrologic type, or degree of aqueous alteration.

Enstatite Chondrites

Carbonaceous Chondrites

SEMARKONA Ordinary NWA 8276 Chondrites NWA 7731 Enstatite Average NWA 10061 Ordinary Average

Carbonaceous Average

3.00 Chondrites

-5 -4 -3 -2 -1 0 1 2 3 4 5 37 δ Cl 45

Figure 1: All Cl isotopic measurement of chondrites compiled from Sharp et al. (2007,2013). Also shown here are the Cl isotopic compositions of all known 3.00 chondrites measured by this work and NWA 8276 from Williams et al. (2015).

Sharp et al., 2015 and Williams et al., 2016 have suggested a new interpretation of the nebular

Cl isotopic composition based on their interpretation of the Martian mantle and a new 3.00-scale chondrite, NWA 8276. These studies present data for the diverse δ37Cl composition of Martian meteorites. All samples that are considered to have been derived directly from the mantle, without incorporation of crustal material, had isotopically-light values of < -2‰. Further, any sample that showed evidence of crustal alteration or assimilation had an isotopically-heavier value. This led to the conclusion that the mantle of Mars has an isotopic composition of ~ -4‰. Sharp et al. 2015 then went on to suggest that this light value of the Martian mantle was likely a primary signature of the source material of Mars itself. All mechanisms that could have altered the isotopic composition of samples derived from the mantle would have raised their isotopic composition.

This was a surprising observation, as the Earth’s mantle and chondrites have a δ37Cl value of 0‰

(Sharp et al. 2013). This means that the mantle of Mars was either sourced from an isotopically- distinct region of the solar nebula, or the Earth and chondrites had become isotopically-heavier through secondary processes.

NWA 8276 has a δ37Cl of -4.5‰, the lightest value of any planetary body measured to date

(Sharp et al 2015). Along with Parnallee, these ordinary chondrites are the only materials that reflect the light values of the Martian mantle. Sharp et al., 2015 explored the idea that these samples

. escaped the incorporation of an HCl-clatherate. HCl-clatherate, with a composition of HCl 3H2O, has previously been proposed by Zolotov and Mironenko 2007 as a Cl ice that forms during the cooling of the solar nebula below ~150 K. Its incorporation into growing asteroidal parent bodies 46 would explain acidic reactions found in CI’s and CM’s such as amorphous silica formation. The

. isotopic fractionation between HCl 3H2Oice and HCl (g) is 3-6‰ (Schauble and Sharp, 2011), so an HCl clatherate condensing out of an HCl gaseous reservoir will have a higher 37Cl value than the reservoir itself. It should be noted that Sharp et al., 2015 did not provide petrographic evidence for this claim.

This study presents the first petrographic evidence supporting HCl-clathrate incorporation into chondrules and other chondrite components. It also reports the Cl isotopic composition for all other known 3.00-scale ordinary chondrites (NWA 10061, NWA 7731, and Semarkona). We have used in situ techniques to map the distribution of Cl in three 3.00 ordinary chondrites, NWA 8276

(L), NWA 10061 (LL) and Semarkona (LL). These samples are critical to the understanding of volatile element incorporation – such as Cl – as they are relatively unaltered samples and yet have very different Cl-isotopic compositions. Identifying the contrasting mechanisms of incorporation within these two samples may shed light on what corresponding nebular conditions may have existed (e.g., regions of HCl-clatherate stability).

2.0 Methods

2.1 Electron microprobe imaging and analyses (EPMA):

An epoxy mount of NWA8276 and a thin section of Semarkona (UNM 549) were acquired from the UNM Institute of Meteoritics collection. Qualitative Cl X-ray maps were made on each section first using the JEOL JXA-8200 Superprobe electron microprobe at UNM to identify areas of interest. Quantitative maps were made for Mg, Na, Al, Si, Ca, Cr, Fe, Cl, S and Ni (Table 1) at

15 kV accelerating voltage, and a 20 nA beam current. Standards for all analyses consisted of a 47 suite of C.M. Taylor Company mineral and synthetic standards, as well as select, in-house mineral standards (Table 1). Background corrections were made using M.A.N. corrections.

Standards (C. M. Taylor

Element Spectrometer Crystal Company)

Mg 3 TapH MgO

Na 3 TapH Albite

Al 1 TapJ Alumina

Si 1 TapJ Quartz

Ca 2 PETL Diopside

Cr 2 PETL Chromite

Fe 5 LiF Hematite

Cl 4 PETH Sodalite

S 4 PETH Pyrite

Ni 5 LiF Nickel metal

Table 1: List of elements collected, crystals and standards used during analytical sessions for quantitative mapping on JOEL microprobe at UNM.

2.2 Scanning Electron Microscope analysis

High-resolution BSE imaging and EDS analysis were performed using the FEI Quanta 3G

FEG-SEM at UNM. The SEM was operated at 10 kV and 16 nA in order to reduce the interaction volume and increase imaging resolution. BSE images were captured at 20 µs/px dwell time.

Mineral phases were identified using qualitative EDS analysis.

2.3 Bulk Mass Spectrometry Analyses

The method for bulk chlorine extraction and analysis used in this study are modified from

Eggankamp (1994). Samples are crushed to a fine powder and leached with 18MΩ H2O for a minimum of four days to remove water-soluble chlorine, which has a high likelihood of containing terrestrial contamination. Sylvite would have been removed from this step, which is discussed in section 3.2.1. After leaching, the samples are melted in an H2O vapor stream (Magenheim et al.1994). The structurally-bound chlorine is volatilized, carried by the H2O vapor stream, and re- condensed as chloride into solution. The aqueous chloride solution is reacted with nitric acid for

12 hours to volatilize any contaminant sulfur and then reacted with AgNO3 to form AgCl(s). The

AgCl is vacuum-filtered using GF/F glass filter paper and dried at 80° C. The AgCl is reacted with excess CH3I in evacuated glass tubes at 80°C for 48 hours to quantitatively convert AgCl to CH3Cl.

Any CH3I and CH3Cl contained in the sealed tube are released into a helium stream using a tube cracker.

Next, the gasses are cryofocused using liquid nitrogen. The gas is then passed through a custom-made glass GC column at 85° C to separate CH3Cl from CH3I. The purified CH3Cl is measured on a Delta XL plus mass spectrometer in continuous flow mode. The flow of gas is reversed as soon as the CH3Cl peak has been analyzed to avoid the introduction of CH3I into the 49

mass spectrometer. The two CH3Cl peaks (mass 50 and 52) are integrated, and the ratio is taken relative to a calibrated internal standard. The long-term external reproducibility of δ37Cl is ±

0.25‰ based on analysis of an in-house seawater standard (Sharp et al. 2007, 2010a, 2010b;

Barnes et al. 2006; Selverstone et al. 2011). The in-house standard used for chlorine isotope measurements is Carmel seawater which we have measured and confirmed is indistinguishable from Standard Mean Ocean Chloride (SMOC) and has a value of 0‰ by definition (Kaufmann

1984).

All Cl isotope measurements are reported in standard delta notation:

δ�� = − 1 ×1000.

3.0 Results

3.1: δ37Cl values of all known 3.00 chondrites

Bulk Cl isotopic measurements for NWA 7731, Semarkona, and NWA 10061 are provided in Table 2 and shown Figure 1. The results for these 3.00, ordinary chondrites (OCs) are very different from the value of NWA 8276, -4.5‰ reported in Sharp et al. (2015). These newly measured 3.00 OCs have δ37Cl near bulk earth (0‰) and average chondrite composition. Cl concentrations were not calculated during this session, as the standards concentrations were not well-calibrated. The error on standard isotopic analysis was ±0.2‰ for this session. 50

Table 2:

Sample δ37Cl (±0.2‰)

Semarkona -0.29

NWA 7731 -0.75

NWA 10061 -0.52

Table 2: Cl isotopic composition of the ordinary chondrites measured by this work.

3.2.1: NWA 8276

A BSE image and qualitative Cl map of NWA 8276 can be seen in figure 2. Epoxy has been masked from these images as it contained high Cl concentrations. Cl concentrations are low and distributed throughout the matrix of the chondrite. Cl is depleted within the chondrules relative to the matrix. All bright spots seen in the Cl map appear to be sylvite on, and in some cases above, the sample surface. The origin of these sylvite growths is unknown, but may be related to sample preparation. No indigenous Cl-bearing phases could be identified as Cl concentrations were too low. 51

Figure 2: Right image: Cl EDS map of 3.00 L NWA 8276. Left image: BSE image of mapping area of sample. All bright spots shown in the Cl map show this sylvite growth

3.2.2: NWA 10061

A BSE image and qualitative Cl map of NWA 8276 can be seen in figure 3. The Cl map shows many areas of high Cl concentrations that are outlined. The area labeled A1, which will be discussed in further detail below, is shown in Figure 4. Figure 4 shows a BSE map and quantitative

EMPA maps of Cl, Fe, and S. A1 is a Fe-Ni metal grain with high concentrations of S as well.

The bulk concentration for the metal was calculated by creating a mask to subtract all data outside of the metal using a custom script in Matlab. The remaining pixels within the chondrule were then averaged. The Bulk composition of the grain can be seen in Table 3. The Cl is found in the core 52 of the metal grain and is heterogeneously distributed. The metal grain has an average Cl concentration of 0.21% with areas as high as 3wt% Cl.

Figure 3: Left image: BSE map for NWA 10061. Right Image: EDS map of Cl.

Figure 4: Quantitative maps of Cl, Fe and S for A1 in NWA 10061 as outlined in Figure 3. Upper left image is a

BSE image of the mapped area.

3.2.3: Semarkona

A BSE image and qualitative Cl map of Semarkona can be seen in Figure 5. This sample shows chondrules and areas with high Cl concentrations, with areas and chondrules outlined in the BSE image (Figure 6). The outlines are labeled 6, 49, A1 and A2. Outlined areas 6 and 49 are Cl- enriched chondrules. Outlined areas A1 and A2 are Cl-enriched areas of interest. Figure 5: 54

Figure 5: Left image: Cl EDS map of 3.00 LL Semarkona. Right image: BSE image of mapping area. Highlighted areas are sections which showed high Cl enrichments relative to the matrix and were quantitatively mapped for Cl.

Each of the outlined chondrules and Cl-enriched areas were quantitatively mapped and can be seen in Figures 6, 8, and 10. Figure 4 shows maps for Cl, Mg, Fe, and Si for Chondrule 6. This type I chondrule has Cl concentrations in the mesostasis interstitial to pyroxene grains as high as

4 wt%. The white outline in the Cl map shows the exterior of the chondrule edge. The outer rim of this chondrule is leached of Cl. There also appears to be a decreasing gradient of Cl concentration from the exterior inward. The bulk composition is presented in Table 3, which was calculated using the same script as that used for NWA 10061, but with all pixels with values of Fe or S (which would indicate metals or sulfides) removed. This chondrule had an average Cl concentration of 973 ppm. 55

Figure 6: Quantitative maps for Cl, MgO ,FeO and SiO2 of chondrule 6. The white outline in the Cl map shows chondrule 6 outline to show that Cl has been leached from the exterior.

Figure 7 shows a BSE image of Chondrule 6 along with two images of regions containing a Cl-rich altered mesostasis. The lower left image represents a typical assemblage in the Cl enriched areas. EDS analysis confirmed that Cl is only in the altered components of the mesostasis

(Ms) and is only found in smectite (Sm). All surrounding phases, including the unaltered mesostasis and pyroxenes (Pyx), contain no detectable Cl. The upper right image shown in Figure

7 also shows that calcite is present as an alteration phase. It is important to note that calcite is not found in the same abundance as smectite. Calcite only appears in a few areas of the chondrule and 56 is not always found in association with smectite. This chondrule is fully encapsulated in a complex sulfide rim seen as the white rind around the chondrule. This sulfide rim contains Fe-Ni metal, magnetite, and sulfide assemblages, and it, too, appears to have undergone alteration.

Figure 7: Upper left image: BSE image of chondrule 6. Upper right image: BSE image of altered mesostasis (Ms) found in chondrule 6 which included calcite and smectite (Sm). Lower Left image: Representative area of mesostasis alteration found throughout chondrule 6 showing mesostasis (Ms) altering to smectite (Sm). The surround pyroxene

(Pyx) contained no Cl. All phases in inset images were identified from EDS spectra.

Figure 8 shows quantitative maps for Cl, Mg, Fe and Si for Chondrule 49. This Chondrule does not show the same degree of Cl enrichment as Chondrule 6, but still contains grains with up to 1.5 wt% Cl. The Cl in Chondrule 49 appears to be zoned with the higher concentrations on the edges, and also has multiple microchondrules accreted on it. The Cl is zoned along this accreted profile. Bulk compositions were calculated in the same manner as those applied to Chondrule 6 and NWA 10061 A1. Average Cl concentrations in this Chondrule were 411 ppm, nearly half of the concentration in Chondrule 6.

Figure 8: Quantitative maps for Cl, MgO ,FeO and SiO2 of chondrule 49.

A sulfide rim also encompasses Chondrule 49, which was also seen in Chondrule 6. This sulfide rim shows alteration as seen in Chondrule 6, Figure 7. Figure 9 shows a BSE image of the sulfide rim surrounding Chondrule 49, where high concentrations of Cl where found. The tricolor

RGB image (Fe, Cl, O) shown is an EDS map of a representative area of the sulfide rim outlined in the BSE map. The core of the image is Fe-Ni metal shown clearly in red, which is surrounded by magnetite-rich areas (purple). The interstitial mesostasis is similarly rich in Cl. The outer edge of this assemblage is a sulfide complex, found ubiquitously along the rim of the chondrule. These sulfide-magnetite assemblages have been previously described (Krot et al., 1997; Singerling et al., in prep) and are thought to be primary (Singerling et al., in prep.). This is similar to the metal grain

(A1) in 10061, which also had high Cl concentrations.

Figure 9:Right image: BSE image of chondrule 49. Beam energy was set to only show high Z phases to outline the

Sulfide rim. The white outlined area was the location of detailed mapping. Upper left image: Three color map, Fe

(red),Cl (green), and O (blue), respectively. Lower left image: BSE image of area shown in upper right image. 59

The other two areas of interest (A1 and A2) highlighted in Figure 5 are shown in Figure

10. A1 appears to be a fragmented chondrule that also contains a sulfide-magnetite assemblage.

A2 is a sulfide assemblage, akin to the sulfide rims surrounding Chondrules 6 and 49. The Cl concentrations in these areas are orders of magnitude higher than the surrounding matrix – as high as 4 wt%. Note that bulk concentrations were not calculated for these regions.

Figure 10: The two upper images are BSE images of A2 (Left) and A1 (right). Lower images are quantitative Cl maps of respective areas.

Table 3:

10061 Semarkona Area 1 Chondrule 6 Chondrule 49 (wt %) (wt %) (wt %) Si 6.60 SiO2 54.15 55.72 S 4.63 SO3 0.1 0.17 Al 0.48 Al2O3 2.33 2.53 Cr 0.19 Cr2O3 0.84 0.77 Fe 40.81 FeO 7.57 8.66 Mg 2.73 MgO 30.71 28.17 Ca 0.93 CaO 1.87 1.75 Na 0.18 Na2O 0.9 0.79 Ni 3.15 NiO 0.48 0.28 Cl 0.21 (ppm) (ppm) Cl 2137 Cl (ppm) 973 411 (ppm)

Total 99.04 98.89 Table 3: Calculated bulk compositions for A1 in NWA 10061 and chondrules 6 and 49 from Semarkona.

Concentrations were calculated using Matlab after masking all areas exterior of the chondrule, removing metals and sulfides and then averaging all remaining pixels. All values are reported as wt% except for Cl which is reported in ppm.

4.0 Discussion

4.1 Summary of Observations in NWA 8276

NWA 8276 indicates very low concentrations of Cl as shown in Figure 2. Cl is also even lower within many of the chondrules. As discussed in section 3.2.1, the only areas of high Cl concentration were found to be surficial contamination which is topographically high. We interpret the low Cl concentrations in this sample as matrix-incorporated Cl from high temperature 61 condensation within the nebula. Perhaps the Cl may have condensed as sodalite, but we were unable to determine at this scale. Future studies may this on the TEM scale to confirm.

4.2 Summary of Observations in NWA 10061

NWA 10061 contains areas of high Cl concentration that stand in great contrast to the distribution observed in NWA 8276. A1 (as shown in Figures 3 and 4) is of particular interest, as it is uncommon to find metals with such high concentration of Cl. The Cl could be bound in a mineral such as Lawrencite. Lawrencite is generally thought to be a product of terrestrial alteration but there have also been studies to suggest that this can be a “primitive” alteration assemblage

(Feng et al. 2012). It is important to note that this study did not do a thorough mineralogical determination of the Cl-bearing phases. However, given the distribution and texture of the Cl within the metal grain shown in A1, the primitive nature of the meteorite, and the similarities to the Cl distributions found in Semarkona (discussed in Section 4.2) , we propose that this the Cl found in this grain represents extraterrestrial alteration. The Cl enrichments found within the grain do not correspond to any depletion in the surrounding matrix. Furthermore, all areas near A1 are homogenously low with respect to Cl. It is therefore likely that the Cl found in A1 was incorporated prior to parent-body accretion.

Many other areas of interest found within this section were not investigated throughout the course of this study, and there is undoubtedly much work left to be done on this particular sample with respect to the Cl distribution.

4.2 A Summary of Observations in Semarkona

As discussed in Section 3.2.2, Semarkona contains chondrules with high concentrations of

Cl (areas with up to 4 wt%). There is a substantial disparity between the Cl enrichments found 62 within the highlighted chondrules and the surrounding matrix (Figures 5, 6, and 9). The alteration phases, in which Cl is found, is only located interior of the respective sulfide rims of both chondrules. The surrounding matrix has low Cl concentrations and no identifiable Cl-bearing phases. This implies either that the Cl was endogenous to the chondrules mesostasis, or that Cl- bearing fluids altered the chondrule prior to parent body incorporation. It seems unlikely that the

Cl was endogenous to the chondrules mesostasis as the unaltered mesostasis (as shown in Figure

7) has no detectable Cl. In addition, none of the surrounding mesostasis or matrix contains Cl or

Cl-bearing phases.

The large enrichments of Cl near magnetite assemblages found within sulfide rims support the idea of alteration local to the chondrule. These complex sulfides have been previously described by Krot et al., 1997 and Singerling et al., in prep. Both studies argue that these assemblages are primary features of the chondrule and predate the parent body assemblage. The rims are thought to be products of liquid immiscibility where the sulfide and metal rich melts are exsolved to the exterior of the chondrule while still in the solar nebula. However, these works did not discuss Cl. The magnetite assemblages in these chondrules as described in Section 3.2.2 and shown in Figure 9 encompass a Fe-Ni core – presumably the precursor material. Surrounding the magnetite assemblage is Cl-rich mesostasis, illustrated in green in Figure 9. This Cl-rich mesostasis extends into the interior of the chondrule. However, the center of the chondrule has very low Cl concentrations (<0.4%), indicating Cl-rich fluid infiltration from the exterior of the chondrule. The same pattern emerges for the concentration gradient seen in Chondrule 6, Figure

6. As was previously mentioned, the Cl in the surrounding matrix of the chondrules is very low and appears to be an unlikely source of Cl. Therefore it is possible that the Cl-bearing fluid that fluxed these chondrules was accreted to those same chondrules prior to parent body incorporation. 63

Cl-enriched areas A1 and A2 shown in Figure 8 are likewise associated with sulfide complexes. A1 is a fragmented chondrule (three pieces) that is adjacent to three sulfide fragments represented as white pieces in the upper right BSE image of Figure 8. The highest Cl concentrations in this area are nearest these two adjacent sulfides (lower and upper right region of

A1). It is important to observe that the interior of the chondrule fragments have no Cl – the Cl only resides in the matrix surrounding the fragments. A2 indicates a fragmented sulfide that is enveloped in Cl-rich mesostasis, yet again demonstrating an apparent connection. It must be noted that not all sulfide rims or fragments found in Semarkona are associated with high concentrations of Cl. But it then follows that the sulfide rims that are associated with high Cl concentrations may present a unique environment in the solar nebula. At this point it is unclear what constitutes this relationship or what the implications may be for the associated formation environments.

4.2: HCl-clathrate mechanism

Cl remains one of the least constrained elements when discussing condensation from nebular gas. The primary gas phases from which it would condense are likely to be: HCl (g),

NaCl(g) or KCl(g) (Lodders and Fegley 1998). It has long been proposed the Cl would condense from these gasses as sodalite with a 50% condensation temperature of 948K (Lodders and Fegley

1998, Lodders 2003). However, primary sodalite has never been found, even in the most pristine chondrites.

The alteration of mesostasis and high Cl concentration found within some chondrules of

Semarkona and NWA 10061 may be associated with the introduction of Cl-rich fluids derived from an HCl-clatherate ice that has been condensed from nebular gas. The formation of an HCl- clathrate ice was first proposed by Zolotov and Mironenko, 2007. This study suggested that 64 clathrate formation would be the primary carrier of Cl in the early solar nebula and could explain the petrographic signatures of acidic reactions observed in some chondrites. Such ice would have a condensation temperature between 140-160K, dependent upon nebular pressure, which is near the predicted H2O ice line. This would move Cl strongly into the volatile field from the previous classification as a moderately-volatile element based on 50% nebular condensation temperatures of 948K. Schauble and Sharp (2011) calculated a theoretical equilibrium Cl isotope fractionation from the condensation of an HCl-clathrate derived from HCl gas to be on the order of 3-6‰ in a nebular environment. In light of this, Sharp et al., (2015) have also suggested that clathrate could be the primary carrier of Cl based on isotopically-light values seen in the chondrites NWA 8276 and Parnallee as well as the Martian mantle. Sharp et al., (2015) hypothesized that the isotopically- heavier values identified in all other chondrite groups and large bodies are the result of HCl- clathrate incorporation that has fractionated from the lighter nebular δ37Cl value of -4‰. This would require the HCl-clatherate ice to be stable through many nebular environments, as the chondrite groups are thought to represent a wide range in nebular conditions (i.e., Cl fugacity, chemistry, and oxygen isotope composition).

We present evidence that the high Cl concentrations found in the detailed chondrules and areas of Semarkona and NWA 10061 presented here align with the proposals of both Zolotov and

Mironenko (2007) and Sharp et al. (2015). The modification proposed here is that the Cl is incorporated into chondrules and other components via HCl-clatherate ice after initial formation, and not as incorporated from parent body processing.

4.3: The Clatherate Model 65

The textures and chemical distribution of Cl in Semarkona and NWA 10061 can be explained through a model of early incorporation of HCl-clatherate (illustrated in Figure 11). We envision the following history: First, chondrules – or other chondrite components – are formed from a melt in the solar nebula. In this stage, the metal rims are formed by the separation of conjugate liquids. During later cooling, the chondrules are incorporated into a larger body, which includes HCl-clatherate ice, presumably together with other dust fragments, chondrules, water ice, etc. Later heating causes Cl-rich acids to alter the chondrules’ metals and mesostasis, alterations that include the oxidation of metal to magnetite and sulfide, and glass to smectite.

During the heating stage, the melting of the ice causes dissociation of the icy body. The altered chondrules are freed and later incorporated into the final chondritic parent body. As stated in Sharp et al. (2015), the formation of this ice would raise the 37Cl value of the parent body as a mass balance of how much ice was incorporated relative to the nebular component shown in

NWA 8276. The lack of alteration in Semarkona and NWA 10061 has allowed for preservation of this primary texture. It very well may be that other chondrites have undergone similar histories, but preservation of this delicate texture is lost during subsequent processing. Smectite breaks down at relatively low metamorphic temperatures and in such a scenario the Cl would be remobilized

(Alexander et al., 1989). Semarkona and NWA 10061 provide a unique opportunity as they have experienced very low degrees of thermal metamorphism. In the same vein, NWA 8276 has also had very low degrees of thermal metamorphism and shows no evidence for clathrate incorporation.

Cl is only found in minor abundances in the matrix and is in lower concentration in the chondrules mesostasis. We interpret the Cl found within NWA 8276 to be nebular Cl incorporated with the matrix material without incorporation of HCl clatherate, thus explicating why NWA 8276 is 66 isotopically light (-4.5‰) (Sharp et al., 2015).

Figure 10: Illustration depicting hypothesis of HCl-clatherate incorporation. Figure reads from left to right. First stage depicts molten chondrules forming sulfide rims. After cooling, chondrules are partially accreted with ice which has some amount of HCl-clatherate. This “dirty ice ball” is then broken apart or the ice is melted freeing the chondrules. The altered, ice bearing, chondrules are then accreted onto a final parent body.

If this mechanism can be extended to other chondrites for halogen incorporation, it may explain the total range of Cl isotopic compositions seen in chondrites even though the averages of the groups are similar. The isotopic composition would be a function of how much nebular Cl, or

Cl from fluids, was incorporated relative to the Cl incorporated by chondrules that contained Cl from an HCl-clatherate ice. 67

4.4 HCl-clatherate incorporation modeling

In addition to being poorly constrained cosmochemically, as previously mentioned, the Cl concentrations of chondritic parent bodies are also poorly defined. Lodders and Fegley 1998 report an average Cl concentration for the LL parent body to be 200ppm. Wasson and Kallemeyn 1988 report the average composition as 100ppm. However, Brearly and Jones (in prep.) show that the

LL chondrites can span Cl compositions of 10 to 300 ppm. Further, there is no correlation in the

LL chondrites between the degree of thermal or aqueous alteration and Cl concentration. For the sake of simplicity in the following model, we will assume that the average of the LL chondrites is

100ppm.

A simple two-component mixing model can be used as a first approximation for the fraction of HCl-clatherate ice incorporated into different chondrite parent bodies. It is assumed that the average Cl concentration of LL ordinary chondrites is 100ppm, as stated above. Because we hypothesize that this is a mixture of nebular Cl (δ37Cl =-4.5‰) and Cl from clatherate ice

(δ37Cl=2‰), we will start the model with an initial Cl concentration of 50ppm nebular Cl. The model then considers the addition of Cl from clatherate ice. Figure 12 illustrates the evolution of this admixture. 68

Figure 12: Figure modeling amount effect of isotopically heavy ice incorporation. Assumptions: Initial Cl concentration= 50ppm(Lodders and Fegley 1998). This figure shows the Cl isotopic composition of the parent body for a given amount of Cl added from HCl-clatherate. The two lines shown are the upper and lower limits of the Cl isotopic composition in all ordinary chondrites measured (Figure 1). This figure also shows the amount of H2O added from the Clatherate from the upper and lower limits of Cl isotopic compositions.

The low-end of the majority of ordinary chondrites – save for NWA 8276 and Parnallee

(Figure 1) – have δ37Cl value is around -2‰. Figure 12 suggests in this model that samples could have 60% of their total Cl incorporated from ice (≈31ppm), to raise the bulk Cl isotopic composition to -2‰. The isotopically-heaviest of ordinary chondrites have δ37Cl values around

1‰. These samples may contain a signal dominated by Cl incorporated by ice, around 550% or 69

270 ppm Cl. As demonstrated in Figure 12, this would constrain the total Cl to between 80 and

320 ppm in the parent body.

As mentioned above, the HCl-clatherate is a hydrated phase with the chemical formula

HCl•3H2O. Therefore, we can use the same model to estimate what the contribution of water would have been from clatherate incorporation. Lodders and Fegley, 1998 report the bulk water composition for LL ordinary chondrites to be 1.1wt%. Figure 12 shows the clatherate could contribute between 0.9 and 7.5% of the total water, based on the Cl added. It may be assumed that the water condensing from nebular H2O gas would also be isotopically heavy. In this context, one might expect that we would see a positive correlation between Cl concentration and isotopic composition in measured samples.

However, Cl in the parent body might be coming from multiple sources during different events. This idea has been discussed in Jones et al. (2014) and Lewis and Jones (submitted). Both of these studies argue for more than one source of Cl in the ordinary chondrite parent- bodies.

These sources could include Cl in matrix and/or mesostasis, or Cl brought in by fluid migration associated with aqueous alteration events and Cl derived from the melting of an HCl-clatherate.

This may have the effect of obscuring the simpler two-component mixing. Further, the lack of isotopic- and concentration-correlation may be influenced by the fraction of ice condensed in different reservoirs within the nebula. The fraction of condensation would indeed affect the isotopic composition of the ice. Due to these complications, we cannot ascertain a unique solution for each measured chondrite. It may be possible to use multiple systems, such as Br and Cl together

– assuming Br also forms a clatherate – to find a closer approximation to the amount of clathrate formation. Future work will be required to constrain the models and hypothesis presented in this manuscript. 70

5.0 Conclusion

This work presents evidence of individual chondrules and other components with very high concentrations of Cl. Similar enrichments were identified by Sharp and Draper 2013 in individual chondrules in the meteorite Qingzhen (EH3) (4.1wt% Cl). In addition, primary sulfide rims were found to encompass the chondrules analyzed herein. The interior alteration of the sulfide rim and chondrules appears to be local and prior to parent body accretion. The Cl found in the alteration assemblages appears to be consistent with the HCl-clatherate formation. This work contributes petrologic evidence for the HCl-clatherate hypothesis presented by Zolotov and Mironenko (2007) and Sharp et al. (2015). Along with a Cl incorporation mechanism, this hypothesis implies that Cl is more volatile in the primitive solar nebula than previously thought, TCondensation Cl=160K. Studies have previously suggested that Cl is depleted in many bodies – including Earth – relative to the volatility trend line in condensation models (Sharp and Draper 2013). However, in the event of a much lower condensation temperature, Cl would be slightly enriched in these bodies relative to the planetary volatility trend.

We present a schematic model for clatherate formation and incorporation into individual chondrules prior to parent body assimilation. This may have important implications for alteration events within chondrules previously recorded through other analyses. In effect, it is unnecessary for the HCl-clatherate to be the only ice accreted onto individual chondrules prior to accretion. In fact, it is likely that water ice would be much more common. Therefore, some aqueous events recorded in the interior of chondrules may also be incorporating water ice that predates parent body assimilation. 71

Our work illustrates that sample heterogeneity is a crucial factor when reporting bulk values of Cl in low-thermal metamorphic grade samples, as there may be some chondrules that dominate the signal. However, at higher grades of thermal and aqueous alteration, the signature of

HCl-clathrate incorporation may be erased as the samples become more homogenous.

Simple modeling of this mechanism serves to show the spread in Cl isotopic composition of chondrites may be attributed to the admixture of Cl from an HCl-clatherate ice and nebular Cl.

The heavier values measured in some samples, relative to an isotopically-light solar nebula, are representative of HCl-clatherate incorporation. Further work should be done to assess the intra- chondrule alteration observed in the Cl-rich chondrules of Semarkona.

Future work should further assess the link between Parnallee and NWA 8276. These samples are the only two chondrites measured to date that preserve the chlorine isotopic composition of the solar nebula. Parnallee, however, has been shown to be Cl-rich (Bridges et al.

2010). Understanding the link between these two samples may further support and refine the conclusions presented herein .

Appendix 1

Bulk H, N and C Isotopic and Concentration Measurements from Water and Organic

Material from Selected Chondrites

This appendix presents preliminary data of H, N, and C from selected chondrites. The methods used to obtain data are described in Alexander et al. 2012. Table one lists all data gathered, blanks indicated no data was collected. This work serves as a preliminary step to future work.

Figures 1 plots all collected data with the data from Alexander et al. 2012. Alexander et al. 2012 used the δD in conjunction with the H/C to approximate the contribution of H from water without an organic component. That is to say that as the H/C approached zero (y-interecept) the measured

H isotopic composition should only be from water. As figure 1 shows this data give new interpretations to the original interpretation of Alexander et al. 2012 for ordinary chondrites (OC),

CV chondrites CO chondrites and CI chondrites. The OC, CV and CO chondrites plot a trend which was not previously seen before which has a y-intercept near 0‰- near Earth . This intercept implies that the CR parent body may share a similar reservoir as the CV’s CO’s and OC’s. It also appears that the CM and CI (including Tagish Lake) parent body share a common water isotopic reservoir which is isotopically light, around -440‰. Further, it appears that Semarkona is an outlier to all groups including the OC’s. To check the validity of this data we measured samples which

Alexander et al. 2012 also measured. Our data agree within error for every duplicate, Table 1.

Bjorbole ZAG NWA8276 NWA7731 NWA10061 Tuxtuax Parnallee Dhajala Karoonda Ornans Kainsaz Allende Vigrano Murray Lake Tagish Orguiel Ivuna

δ 15 N (‰) N

- - - - - 19.7 25.3 13.1 37.8 46.3 45.2 31.9 47.2 36.3 39.9 - - - - 2.2 1.8 9.5 5.1 1.7 2.7 4.0

(ug/g) Concentration

1021 1965 2178 2705 408 155 116 501 208 101 259 13 16 80 18 20 7

(‰) δ 13 C ------23.4 22.9 17.6 12.9 18.5 22.8 25.4 26.5 23.8 15.6 17.4 18.7 15.8 12.9 11.8 -

7.7 8.1

(ug/g) Concentration

10730 20257 41137 40253 38886 4269 1709 4985 7974 1972 9134 1048 815 758 803 966 876

δ D (‰)D

- 107 154 604 277 - - - - - 71 73 10 94 22 75

(ug/g) Concentration

12304 1304 1727 8489 8291 174 377 130 185 252

Table 1: N, C and H isotopic compositions and concentrations for measured samples

Figure 1: Hydrogen isotopic composition vs C/H ratios for measured samples combined with data from Alexander et al. 2012. Black lines represent best fit regressions for clusters of chondrite classes

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