Provenance and distribution of zinc in terrestrial planets

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Morton, Yihang Huang, Helen M. Williams, and 1 more This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-6888308/v1 This work is licensed under a CC BY 4.0 License Status: Published Journal Publication published 18 Nov, 2025 Read the published version in Scientific Reports → Version 1 posted 11 You are reading this latest preprint version Abstract Analyses of Earth’s nucleosynthetic Zn isotope composition indicate that its inventory of this volatile element was derived from a mixture of materials originating in both the inner and outer regions of the Solar System. In contrast, the nucleosynthetic Zn isotope composition of Martian meteorites suggests that, despite being more volatile-rich than Earth, Mars received very limited Zn from outer Solar System sources. Modeling for Earth also indicates that, although only ~30% of its mass was supplied by chondritic material, such undifferentiated, primitive bodies contributed ~90% of its Zn. However, the total chondritic contribution to Mars, and its role in shaping the planet’s volatile budget, remain poorly constrained. Here, we present nucleosynthetic Zn isotope data for six Martian meteorites, confirming that Mars’ Zn was likely sourced exclusively from inner Solar System material. These data were incorporated into a comprehensive mixing model that includes constraints from eight additional isotope systems and major element abundances. The results are consistent with Mars having accreted ~50% of its mass from chondritic material, which also delivered ~90% of its Zn. Together, these findings suggest that the proportion of undifferentiated material accreted by a planet plays a more critical role in establishing its volatile budget than the specific provenance of the accreting sources. Finally, we report mass-independent Zn isotope compositions for five Lunar samples. The results are indistinguishable, within uncertainty, from values for the bulk silicate Earth (BSE) and non-carbonaceous (NC) meteorites. Further analyses are thus required to reliably constrain the origin of Lunar Zn. Earth and environmental sciences/Planetary science/Early solar system Physical sciences/Astronomy and planetary science/Planetary science/Inner planets Figures Figure 1 Figure 2 Figure 3 Figure 4 Introduction Constraining the origins of volatiles in terrestrial planets is essential for understanding their formation and how they become habitable. Recent nucleosynthetic isotope studies showed that Earth’s inventories of the moderately volatile elements Zn and K are derived from mixed sources, including both NC planetesimals that formed locally as well as material akin to carbonaceous chondrites (CCs) that originated from much greater heliocentric distances 1-4 . Accretion of primitive material, which survived melting and differentiation in the early Solar System, has also been shown to play a crucial role in establishing Earth’s volatile content 5 . Nonetheless, it is unclear whether these features are common across terrestrial planets, or whether Earth presents a special case. While Mars’ Zn budget was supplied primarily by locally sourced NC material 6,7 , the contribution of primitive material to Martian volatiles remains unconstrained. Early work attempted to explain Mars’ volatile content by mixing different nebular components with variable volatile abundances 8,9 . However, studies that reproduced the isotope composition of Mars by mixing of different chondritic endmembers typically resulted in bulk elemental compositions that were too volatile-rich 10-12 . Importantly, the extent of volatile depletion exhibited by a planet or planetesimal may not exclusively reflect nebular processes, as substantial volatile loss can occur during accretion. Heat derived from the decay of extinct radionuclides can produce enough energy to induce the formation of magma oceans in small, differentiated planetesimals, which allows for effective volatilization and degassing 13 . These processes furthermore produce mass-dependent isotope fractionations consistent with those observed in some planetesimals 14,15 . Therefore, planets accrete from a mixture of differentiated and undifferentiated materials, which likely shapes their volatile inventories. Albeit not directly, the composition and volatile content of a third terrestrial body can be investigated – Theia, the Mars-sized planet that likely collided with proto-Earth to form the Moon 16 . Theia’s existence is inferred from the giant impact hypothesis – the most prominent theory for the formation of the Moon 17,18 . This scenario calls for a collision between proto-Earth and Theia, leading to the formation of the Moon from the magma disk generated after impact. While the Moon is thought to have been primarily formed from the impactor, Theia’s composition remains elusive, as it cannot be directly accessed. Nonetheless, the similarities between the nucleosynthetic isotope compositions of the Earth and Moon 19-22 have been inferred to also extend to Theia. Due to their substantial volatile depletion, and considerable analytical challenges associated with measuring such limited samples, no nucleosynthetic isotope compositions of volatile elements are currently available for Lunar samples. The origin of volatiles for the Moon and Theia thus remain unconstrained. Results Here, we present mass-independent Zn isotope results for Martian and Lunar samples. The terrestrial rock reference material BCR-2, which was analysed concurrently for quality control, is indistinguishable in εZn from the London Zn isotope standard (Table 1, Fig. 1). In contrast, all Martian meteorites display resolvable anomalies relative to the terrestrial composition, yielding results for bulk silicate Mars (BSM) in agreement with previous data 6,7 (i.e., e 66 Zn BSM = -0.15 ± 0.04, 2se). Our accompanying results for the CI meteorite Orgueil are also consistent with previously published values for this meteorite (Table 1). Due to the limited sample masses and their severe Zn depletion, the analyses of the Lunar samples used run solutions with Zn concentrations as low as 150 ng g -1 (compared to up to 500 ng g -1 for other samples), employed fewer data acquisition cycles, and encompassed fewer repeat runs than were obtained for other samples. This resulted in isotope data with larger uncertainties compared to the other results presented in this study (Table 1). The results for 15016-254 and 70017-587 are indistinguishable from terrestrial Zn and NC meteorites (e 66 Zn = -0.10 ± 0.30 and -0.11 ± 0.07, respectively; Table 1, Fig. 2). In contrast, NWA 11898 displays resolvable negative anomalies relative to the terrestrial mean within ±2se (e 66 Zn = -0.29 ± 0.06), while NWA 11182 and 10017-423 display resolvable positive anomalies (i.e.: e 67 Zn = 0.40 ± 0.11 and 0.44 ± 0.21, respectively). Finally, the mean obtained for the five Lunar samples (i.e., e 66 Zn Lunar = 0.01 ± 0.19; 2se) overlaps with previously attained values for the BSE and NC chondrites 1 (NCCs; Fig. 1). Discussion Lunar samples Lunar samples display identical mass-independent isotope compositions to the BSE for several isotope systems, such as O, W, Ca, Ti, and Cr 19-24 . Despite these similarities, dynamical models of the giant impact suggest that proto-Earth’s contribution to the Moon was limited, with approximately 70–80% of the Lunar mass being derived from the giant impactor 16,25 . Combined, these observations may imply that the isotopic similarities also extended to Theia. However, the likelihood of an accretion scenario where Theia was isotopically identical to the BSE for most isotope systems is minimal, with one study estimating that there is less than a 1% chance for Theia and Earth to accrete with indistinguishable W and O isotope compositions 26 . Importantly, the concentrations of non-volatile elements are very similar between CCs, NCCs, and differentiated meteorite parent bodies 27-31 . This contrasts with the distribution of volatile Zn, as this has highly variable abundances in different bodies, with concentrations ranging from less than 1 mg g -1 in some meteorites from differentiated NC parent bodies (DNCs) to over 300 mg g -1 in some CCs and NCCs 27-31 . Hence, even if Theia accreted from the same proportions of CCs, NCCs and DNCs as Earth, this could still result in a distinct nucleosynthetic Zn isotope composition, if the accreted materials differed in their Zn concentrations. In other words, two planets that share the same nucleosynthetic Zn isotope signature can only be generated if both the Zn isotope compositions and abundances of the accreting materials were essentially identical, and this constitutes a very unlikely scenario. An equally improbable explanation is that Theia and Earth accreted from different materials, which coincidently produced the same final bulk nucleosynthetic isotope composition. Hence, similar nucleosynthetic Zn isotope compositions for the Moon and the BSE would place even more significant constraints on the giant impact scenario. The improbability of a scenario where Theia was isotopically identical to the BSE led to the hypothesis of post-impact homogenization 26 . This scenario allows for distinct compositions for the impactor and the BSE, which would have been homogenized through vapor-phase equilibration between Earth’s mantle and the magma disk from which the Moon formed. Previous studies have shown that this scenario is feasible even for refractory elements, such as Ti 22 . Such a process should therefore inevitably affect Zn, which is volatile and, hence, more susceptible to vaporization and re-equilibration. The five Lunar samples display variable compositions, ranging from e 66 Zn = -0.29 ± 0.06 to e 66 Zn = 0.29 ± 0.39 (2se) (Fig.1, Table 1). All samples furthermore present a well-defined correlation between e 66 Zn and e 67 Zn values (R 2 = 0.98; Fig. 2). Importantly, the slope of this correlation is incompatible with variations predicted for nucleosynthetic isotope anomalies originating from either electron capture core collapse (ECSNe) or Type Ia (SN Ia) supernovae, which have been shown to be consistent with anomalies of other Solar System materials 1 (Fig. 2). It is hence likely that the observed variations reflect other processes that can affect mass-independent Zn isotope compositions. Results of previous studies suggest that the mass-dependent Zn isotope compositions of Lunar samples were affected by kinetic isotope fractionation associated with evaporative Zn loss 32 . As such, it is possible that the exponential law, which was employed in the internal normalization procedure used here, did not adequately correct for the extent of kinetic mass-dependent isotopic fractionation experienced by some of the samples. The mass-dependent isotope compositions of the samples were thus calculated according to Eq. (S1). Importantly, these results were not obtained using the same method that was applied for the Martian samples (see SI) and are reported relative to the London Zn standard rather than JMC Lyon Zn standard. As such, the Lunar d 66 Zn values are accompanied by larger uncertainties and may not exclusively reflect the natural composition of the samples, but also potentially isotope fractionation incurred during the analytical procedure. Nonetheless, they can be useful to assess whether any correlation between the extent of mass-dependent fractionation and the mass-independent results can be detected. The two samples with indistinguishable positive mass-independent isotope anomalies – 10017-423 and NWA 11182 – display clearly distinct mass-dependent isotope compositions, with mean d 66 Zn values of -6.05‰ and 0.82‰, respectively (Fig. S1). Similarly, the two samples that are indistinguishable from the BSE in e 66 Zn (15016-254 and 70017-587) have markedly distinct mass-dependent isotope compositions (d 66 Zn of -0.69‰ and 8.99‰, respectively). Finally, the only sample that displays a negative e 66 Zn anomaly (NWA 11898) is very fractionated (d 66 Zn = 9.04‰), with a mass-dependent isotope composition that that is comparable to that of 70017-587. Hence, the variability in mass-independent isotope composition does not appear to be influenced by mass-dependent isotope fractionation. All samples are derived from the Lunar surface, where they can be exposed to galactic cosmic rays, which could, in principle, alter Zn isotope compositions. Whilst still comparatively small, 67 Zn has the largest neutron capture cross-section among the five Zn isotopes, and cosmogenic reactions could hence decrease the abundance of 67 Zn through an induced (n,γ) reaction to produce 68 Zn. The potential effects of this process can hence be most readily assessed by examining the e 67 Zn values determined for the samples. Although sample 10017-423 displays the largest offset from the mean (e 67 Zn = 0.44 ± 0.21, 2se) and the highest cosmogenic exposure age (480 ± 70 Ma) 33 , the positive e 67 Zn value is the opposite of what would be expected for a decrease in the abundance of 67 Zn caused by cosmogenic effects. Furthermore, the two other Apollo samples with identical e 67 Zn values (e 67 Zn = 0.03 ± 0.07; e 67 Zn = 0.02 ± 0.16) have clearly distinct cosmogenic exposure ages (315 ± 20 and 220 ± 20 Ma, for 15016 and 70017, respectively) 34,35 (Fig. S1). Therefore, even if present, the effects of cosmogenic exposure on the mass-independent Zn isotope compositions of the analyzed samples are unlikely to be resolvable within the obtained precision. Samples from the Lunar surface may also be contaminated by local impacting material that originates from isotopically distinct bodies. Previous studies found no substantial evidence for variations in the nucleosynthetic isotope composition of Lunar samples for other isotope systems 19-23 . However, Zn may be more susceptible to such alteration due to the severe Zn depletion recorded by the Moon. Nonetheless, as stated previously, the compositions of the Lunar samples define an excellent correlation, with a slope that is clearly distinct from the nucleosynthetic isotope variations predicted for the potential sources of the nucleosynthetic Zn anomalies (Fig. 2). The variability in the mass-independent Zn isotope composition of the Lunar samples is therefore unlikely to reflect contamination from isotopically distinct materials. Equally, the results are incompatible with modeled compositions for mass-independent isotope fractionation caused by the nuclear field shift effects (Fig. 2) 1 . Finally, it is possible that the eZn data obtained for some samples are affected by isobaric or molecular interferences, or matrix effects. To test this, exploratory elemental analyses of sample solutions used for the Zn isotope analyses were performed using an iCAP Q inductively coupled plasma mass spectrometer (ICP-MS) at the University of Cambridge. Small aliquots of the three Apollo samples, Orgueil, and BCR-2 were taken after the Zn purification procedure. No systematic differences were detected between any of the samples, which display concentrations comparable to the blank for all fifty-seven elements that were analyzed. An aliquot of sample 10017-423 was furthermore subjected to a digestion protocol employing hydrogen peroxide in an attempt to eliminate organics possibly leached from the resins utilized in the ion exchange procedure 36 . This resulted in no detectable differences in the mass-independent isotope composition of this sample (e 66 Zn = 0.58 ± 0.18; e 67 Zn = 0.53 ± 0.10) from the mean obtained for aliquots that were not subjected to this procedure (e 66 Zn = 0.22 ± 0.46; e 67 Zn = 0.42 ± 0.26). Hence, while it is unclear which processes are recorded by the mass-independent Zn isotope composition of the Lunar samples in this study, it is unlikely that they all reflect the nucleosynthetic isotope composition of the Moon. As the only samples consistent with predicted nucleosynthetic isotope compositions, 15016-254 and 70017-587 are the least likely to have been affected by other processes and may in fact reflect the nucleosynthetic Zn isotope composition of the Moon. If so, this would define a mean nucleosynthetic Zn isotope composition for the Moon that is indistinguishable from the BSE (e 66 Zn = -0.11 ± 0.30; e 67 Zn = 0.02 ± 0.17), in line with findings for other isotope systems. However, with the available precision, the results are also indistinguishable from NCs (Fig. 1). Further analyses are hence required to confirm whether no distinctions can be resolved between the Lunar samples and the BSE. Martian samples As for non-volatile elements, the Martian samples analyzed in this study display resolvable nucleosynthetic Zn isotope anomalies relative to the BSE (e 66 Zn BSM = -0.15 ± 0.05; 2se), in line with previous studies 6,7 . The results for Mars furthermore overlap with data for NCCs 1,3,4 (Fig. 2). To estimate the CC contribution to Mars’ Zn inventory, mixtures between different meteorite groups were modelled using a Monte Carlo simulation with 10,000 trials. In the first trial, all groups for which nucleosynthetic Zn isotope compositions are available were included (Supplementary Information). For each trial, the endmembers were randomly selected, and their compositions were generated in a normal distribution within the adopted values, along with arbitrary mass fractions between 0 and 100%. The final compositions of the mixtures were calculated by mass balance but only results which yielded Mars-like e 66 Zn values were selected (e 66 Zn BSM = -0.15 ± 0.03, 2se; Table 1). Most successful trials (63%) correspond to mixtures where no CCs were included, indicating that Mars’ nucleosynthetic Zn isotope composition can be more readily reproduced by exclusively incorporating NC material (Fig. 3). The average CC-like Zn for all successful trials is ~16%, with 35% of them falling in the range ~1-20%. These results are in agreement with previous models which estimated a CC Zn contribution to Mars of ~23% 6 and up to ~22% 7 . However, differentiated materials have been estimated to have supplied just ~10% of Earth’s Zn 5 . Since their contribution is likely very limited, another run of the model was performed where only chondritic groups were included as endmembers. In this case, 43% of successful trials included no CCs, and 51% included between 1-20% CC-like Zn. As such, the inclusion of differentiated meteorite groups had only minor effects on the outcome of the model. For comparison, the same models were applied to the BSE (e 66 Zn = -0.03 ± 0.03, 2se). When all groups were included, trials with ~20-65% CC-like Zn were successful, with most results falling at ~40%, in line with previous studies 1,3,5,7 . In the run that employed only chondrites, most of the successful trials fall between ~15-55%, with maximum probability at ~36% CC material (Fig. 3). In either case, this defines a much more substantial CC contribution to the BSE than to BSM, since the latter appears to have received only a negligible Zn contribution from material with a CC origin. In addition to constraining the Zn contribution from CC materials, we also employed our results in a more comprehensive model to identify the main building blocks accreted by Mars. To do so, elemental concentrations were modelled for ten major elements (Na, Mg, Si, P, Ca, K, Ti, Fe, and Mn) and isotope compositions for nine isotope systems (Δ 17 O, ɛ 48 Ca, ɛ 50 Ti, ɛ 54 Cr, ɛ 64 Zn, ɛ 84 Sr, ɛ 96 Zr, d 30 Si and d 25 Mg) using the approach described in detail in Martins et al. 5 . The models employed Monte Carlo simulations with variable numbers of trials depending on the run (Table 2). To allow for a direct comparison with previously reported results for the BSE 5 , the same parameters and data were employed, including the use of ɛ 64 Zn values internally normalized to the 66 Zn/ 67 Zn ratio (Table S2). All relevant literature data for Mars summarized in Tables S3 and S4 (Supplementary information). The endmembers included CC (CI, CM, CV, CO) and NCC (H, L, LL ordinary chondrites and EH, EL enstatite chondrite) meteorite groups, as well as the parent bodies of two non-carbonaceous achondritic meteorites – eucrites and angrites (EPB and APB, respectively), which are derived from differentiated non-carbonaceous (DNC) planetesimals. The endmembers were randomly selected and assigned arbitrary mass fractions for each of the trials. Their isotope and elemental compositions were randomly generated within the compiled literature values 5 . The resulting compositions of the mixtures were calculated by mass balance and the selection of valid results varied between runs. The mass fractions of each endmember and the resulting isotope compositions are reported as mean values and twice the standard deviation, based on all valid trials for each run. For the elemental abundances, the highest and lowest values obtained in valid runs are presented in Fig. 4. A total of four runs were performed, with each featuring distinct criteria for the selection of valid solutions (Table 2). For the first run of the model, only trials that yielded Mars-like mass-independent isotope compositions were selected (Δ 17 O, ɛ 48 Ca, ɛ 50 Ti, ɛ 54 Cr, ɛ 64 Zn, ɛ 84 Sr, and ɛ 96 Zr), and this resulted in a mixture comprised mainly of NCCs (87 ± 17%) with much more limited fractions of CCs (4 ± 3%), and DNC material (13 ± 11%). However, this produced elemental abundances that are inconsistent with literature estimates for Mars, with noticeable excesses of volatile elements (e.g., Na, P, K). The elemental abundances were successfully reproduced by Run 2, which produced a smaller NCC fraction (44 ± 29%) combined with larger contributions from CCs ( %) and DNCs (44 ± 27%). The solutions resulting from this run, however, produced a wide range of mass-independent isotope compositions that were not compatible with literature values. Nonetheless, the mass-dependent d 30 Si and d 25 Mg values of these mixtures were consistent with literature results for Mars. Finally, no combination of these materials could reproduce both the Martian isotope compositions and the elemental abundances in Run 3. Combined, the results of Runs 1, 2, and 3 therefore imply that, in addition to CCs and NCCs, Mars likely accreted a significant fraction of DNC material that had NCC-like nucleosynthetic isotope compositions. One known DNC body was sampled by aubrites, a group of meteorites thought to originate from a differentiated enstatite chondrite-like planetesimal 37 . However, some of the data needed to characterize the endmember composition of this DNC meteorite group are unavailable 5 . Thus, in Run 4, hypothetical unsampled materials were adopted as DNC endmembers. In detail, these materials were characterized by the elemental abundances and mass-dependent isotope compositions of the APB and EPB, but the mass-independent isotope compositions of ordinary and enstatite chondrites, respectively, for Unsampled Materials 1 and 2 (UM1 and UM2). As such, UM1 and UM2 are equivalent to DNC enstatite and ordinary chondrite planetesimals, respectively 5 . With these parameters, Run 4 reproduced the isotope and elemental compositions of Mars with 53 ± 23% of DNC, 47 ± 23% of NCC, and 1 ± 1% of CC material (Table 2, Fig. 4). The Run 4 results highlight a significant difference in the CC contributions to Earth (10 ± 3%) 5 and Mars (1 ± 1%) (Table 2, Fig. 4). Yet, the abundances of most volatile elements are higher for Mars than for Earth 38 . The results thus demonstrate that, while CCs may have played a substantial role in establishing Earth’s volatile inventory, material derived from a colder, volatile-rich region of the Solar System is not required to build a volatile-rich terrestrial planet. Instead, the more important determining factor appears to be the accretion of undifferentiated chondritic material, regardless of its origin within the Solar System. This chondritic material (NCC and CC combined) contributed ~30% and ~50% to the masses of Earth and Mars, respectively, but critically provided ~90% of the Zn inventories to both planets. The remaining accreting material was comprised of differentiated, volatile-poor planetesimals, which supplied just ~10% of the Zn. Methods Samples and sample preparation The study investigated three Apollo Lunar samples, two Lunar meteorites, and six Martian meteorites (Table 1). Digestion and preparation of the samples and the subsequent Zn isotope measurements were carried out in the MAGIC Laboratories at the Department of Earth Science & Engineering of Imperial College London, following the procedures outlined in Martins et al. 1 . All sample preparation was conducted in ISO Class 6 clean rooms, using ISO Class 4 laminar flow benches for critical steps. The water used was of ≥ 18.2 MΩ cm quality from a Millipore purification system. All acids were purified from reagent grade stock acids by sub-boiling distillation in either quartz glass (15.3 M HNO 3 , 6 M HCl) or Teflon (28 M HF, 12 M HCl, 8.5 M HBr) stills. The samples were completely crushed with an agate mortar and pestle and digested in Savillex Teflon beakers. The digestion procedure started with refluxing in a 2 + 1 mixture of 28 M HF + 15.3 M HNO 3 at 120 °C for at least two days on a hotplate, followed by evaporation to dryness. This process was then repeated with 6 M HCl. Following digestion, the samples were purified using the three-stage anion exchange procedure described in Martins et al. 1 . Mass-independent Zn Isotope measurements The isotope analyses were conducted with a Nu Instruments Nu Plasma II multiple collector inductively coupled plasma mass spectrometer (MC-ICP-MS). A Nu Instruments DSN 100 desolvation system fitted with glass cross flow nebulizers with solution flow rates of about 120 μl min -1 were employed for sample introduction in conjunction with a CETAC ASX 112FR autosampler. The analytical procedures followed the methods described in Martins et al. 5 . Most samples were analysed using two cup configuration 1 . However, samples with limited Zn were occasionally analysed using a single cup configuration and without performing a correction for Ge interferences on 70 Zn 5 . All ion beams were monitored using Faraday cups fitted with 10 11 Ω resistors. Each run was started by a peak centering routine, whilst each block commenced with a 60 s measurement of the electronic baselines of the Faraday collectors whilst the ion beam was deflected in the electrostatic analyser. Data acquisition for the Martian samples encompassed 3 blocks with 20 measurement cycles of 8 s each. Due to the low Zn contents of the Lunar samples, their analyses encompassed only 2 blocks with 20 data acquisition cycles. The samples were introduced as solutions in 0.1 M HNO 3 , typically containing 150-500 ng g -1 of Zn, with instrumental sensitivity ranging between 150 and 350 V (µg ml -1 ) -1 . All sample analyses were carried out with the sample–standard bracketing technique, in which sample runs were symmetrically bracketed by runs of the London Zn isotope reference material. The Zn concentrations of the latter were matched to the sample concentrations to within 10 to 15%. The Zn isotope results are reported using the ε notation, which denotes deviations of the measured isotope ratio for a sample (sam) from the value determined for the London Zn reference standard (std) in parts per 10 4 : where i/68 is the isotope ratio of interest and the 64 Zn/ 68 Zn ratio that was used for internal normalization with the exponential law. Additional results obtained using 66 Zn/ 67 Zn for internal normalization are reported in the Supplementary Information (Table S2). Declarations Acknowledgements We are grateful to the NASA Johnson Space Center (R. Zeigler) for providing the Apollo samples, and the Natural History Museum London for the Orgueil sample. The US Antarctic meteorite samples are from the Antarctic Search for Meteorites (ANSMET) program; they are curated by the Dept. of Mineral Sciences of the Smithsonian Institution and the Astromaterials Curation Office at NASA Johnson Space Center. We also thank Jason Day and Helena Pryer for their assistance in the laboratory. This work was funded by an Imperial College London President’s PhD Scholarship (R.M.), an ERC Advanced grant 101020665 (R.M., H.M.W.), an UKRI STFC grant ST/W001179/1 (M.R., E.M.M.). Author contributions M.R. designed the research. R.M., E.M.M. and Y.H. performed the sample preparation and analyses. R.M. performed the modeling. All authors contributed to interpretation. R.M. wrote the first draft of the manuscript, which was subsequently edited by all authors. Competing interests The author(s) declare no competing interests. Data availability All data generated or analysed during this study are included in this published article (and its supplementary information files). References Martins, R., Kuthning, S., Coles, B. J., Kreissig, K. & Rehkämper, M. Nucleosynthetic isotope anomalies of zinc in meteorites constrain the origin of Earth’s volatiles. Science 379 , 369-372 (2023). Nie, N. X. et al. 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High precision zinc stable isotope measurement of certified biological reference materials using the double spike technique and multiple collector-ICP-MS. Anal. Bioanal. Chem. 409 , 2941–2295 (2017). Keil, K. Enstatite achondrite meteorites (aubrites) and the histories of their asteroidal parent bodies. Geochemistry 70 , 295-317 (2010). McSween, H. Y. & McLennan, S. M. in Treatise on Geochemistry (Second Edition) (eds Heinrich D. Holland & Karl K. Turekian) 251-300 (Elsevier, 2014). Bridgestock, L. J. et al. Unlocking the zinc isotope systematics of iron meteorites. Earth Planet. Sci. Lett. 400 , 153–164 (2014). Pickard, H. et al. The cadmium and zinc isotope compositions of the silicate Earth – Implications for terrestrial volatile accretion. Geochim. Cosmochim. Acta 338 , 165-180 (2022). Archer, C. et al. Inter-calibration of a proposed new primary reference standard AA-ETH Zn for zinc isotopic analysis. J. Anal. At. Spectrom. 32 , 415-419 (2017). Paniello, R. C., Day, J. M. D. & Moynier, F. Zinc isotopic evidence for the origin of the Moon. Nature 490 , 376-379 (2012). Doucet, L. S. et al. Archean lithospheric differentiation: Insights from Fe and Zn isotopes. Geology 48 , 1028-1032 (2020). Fang, S.-B. et al. Zinc isotope fractionation in mantle rocks and minerals, and a revised δ66Zn value for the Bulk Silicate Earth. Geochim. Cosmochim. Acta 338 , 79-92 (2022). McCoy-West, A. J., Fitton, J. G., Pons, M.-L., Inglis, E. C. & Williams, H. M. The Fe and Zn isotope composition of deep mantle source regions: Insights from Baffin Island picrites. Geochim. Cosmochim. Acta 238 , 542-562 (2018). Sossi, P. A., Nebel, O., O'Neill, H. S. C. & Moynier, F. Zinc isotope composition of the Earth and its behaviour during planetary accretion. Chem. Geol. 477 , 73-84 (2018). Liebske, C. & Khan, A. On the principal building blocks of Mars and Earth. Icarus 322 , 121-134 (2019). Rüfenacht, M. et al. 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Adv. 10 , eadl1007 (2024). Tables Table 1. Mass-independent Zn isotope data (in εZn notation) for meteorite, Martian, Lunar and terrestrial samples. Sample name Type Mass (g) e 66 Zn 2sd 2se e 67 Zn 2sd 2se n MIL 03346 Nakhlite 0.310 -0.26 0.32 0.12 0.05 0.32 0.12 7 ALH 77005 Shergottite 0.290 -0.10 0.26 0.09 0.04 0.42 0.15 8 EET 79001 Shergottite 0.300 -0.20 0.23 0.09 -0.03 0.39 0.16 6 LAR 12095 Shergottite 0.300 -0.08 0.21 0.07 0.16 0.21 0.08 7 RBT 04262 Shergottite 0.300 -0.14 0.18 0.07 0.06 0.22 0.09 6 ALH 84001 SNC OPX 0.300 -0.12 0.23 0.07 0.10 0.32 0.09 12 BSM -0.15 0.12 0.05 0.06 0.12 0.05 6 70017-587 High-Ti Mare Basalt 1.898 -0.11 0.21 0.07 0.03 0.22 0.07 9 10017-423 High-Ti Ilmenite Basalt 0.400 0.29 0.87 0.39 0.44 0.48 0.21 5 15016-254 Low-Ti Olivine Basalt 2.400 -0.10 - 0.30 0.02 - 0.17 2 NWA 11182 Feldspathic breccia 2.000 0.18 - 0.19 0.40 - 0.11 2 NWA 11898 Feldspathic breccia 2.050 -0.29 0.13 0.06 0.17 0.08 0.04 4 Lunar mean -0.01 0.43 0.19 0.14 0.48 0.21 5 Orgueil CI 0.32 0.24 0.06 -0.07 0.25 0.06 18 BCR-2 Terrestrial 0.00 0.26 0.04 0.00 0.27 0.05 34 n is the total number of individual analytical runs for a given meteorite, for one or several powder/digest solution aliquots. Table 2. Summary of results from the Monte Carlo simulations for the building blocks of Mars. Run 1 2 3 4 Nucleosynthetic isotope composition ✓ ✓ ✓ Major elements ratios ✓ ✓ ✓ Endmembers CC, NCC, APB, EPB CC, NCC, APB, EPB CC, NCC, APB, EPB CC, NCC, UM1, UM2 Trials 10 8 10 4 10 8 10 8 Solutions 478 2428 0 787 CC (%, ± 2sd) 4 ± 3 - 1 ± 1 NCC (%, ± 2sd) 87 ± 17 44 ± 29 - 47 ± 23 APB/EPB/UM (%, ± 2sd) 13 ± 11 44 ± 27 - 53 ± 23 Checkmarks indicate literature values for Mars that are successfully reproduced by each run. Meteorite groups included in the models: CI, CM, CO, CV, EH, EL, H, L, LL, eucrite parent body (EPB), angrite parent body (APB), and Unsampled Materials 1 and 2, UM1 and UM2. UM1 and UM2 have eucrite- and angrite-like elemental abundances and mass-dependent isotope compositions, but OC and EC-like nucleosynthetic isotope compositions, respectively, following Martins et al. 5 . Additional Declarations No competing interests reported. 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Also discoverable on Platform About Our Team In Review Editorial Policies Advisory Board Help Center Resources Author Services Accessibility API Access RSS feed Manage Cookie Preferences © Research Square 2026 | ISSN 2693-5015 (online) Privacy Policy Terms of Service Do Not Sell My Personal Information {"props":{"pageProps":{"initialData":{"identity":"rs-6888308","acceptedTermsAndConditions":true,"allowDirectSubmit":false,"archivedVersions":[],"articleType":"Article","associatedPublications":[],"authors":[{"id":471144522,"identity":"df80ed41-2aa2-4df1-bec6-e4c7c0ef4721","order_by":0,"name":"Rayssa Martins","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAAwUlEQVRIiWNgGAWjYFAC5gMHPv6xgXMNiNDClnhwZkMaSVp4jA/zNhwmQYv5tAMGB2fuOC/PP+0A44cfDIeNCWqRuZ2QcODjmduGM24nMEv2MBw2I6hFQjrhwMEZbLcTGIBImoHhsA0RWhIbDvOwnUuQB9rym0gtyQyHedsOJBjcTmAD2UKMw9IYDs44k2y48XZim2WPQTph70tI53/+8KHCTl7udvLhGz8qrA0bCOpBAMYG4iJyFIyCUTAKRgFhAAC1Xz7O9OUVxAAAAABJRU5ErkJggg==","orcid":"","institution":"Imperial College London","correspondingAuthor":true,"prefix":"","firstName":"Rayssa","middleName":"","lastName":"Martins","suffix":""},{"id":471144523,"identity":"890a7bbc-819a-44f1-8ade-e137219db49e","order_by":1,"name":"Elin M. Morton","email":"","orcid":"","institution":"Imperial College London","correspondingAuthor":false,"prefix":"","firstName":"Elin","middleName":"M.","lastName":"Morton","suffix":""},{"id":471144524,"identity":"7a329c70-bdb7-465a-b505-3ff42f31d5ae","order_by":2,"name":"Yihang Huang","email":"","orcid":"","institution":"Imperial College London","correspondingAuthor":false,"prefix":"","firstName":"Yihang","middleName":"","lastName":"Huang","suffix":""},{"id":471144525,"identity":"ccd64e3d-1a85-4f5f-82cf-77d6f0368a2a","order_by":3,"name":"Helen M. Williams","email":"","orcid":"","institution":"The University of Cambridge","correspondingAuthor":false,"prefix":"","firstName":"Helen","middleName":"M.","lastName":"Williams","suffix":""},{"id":471144527,"identity":"21b0406b-8941-436c-abe1-d5418742004e","order_by":4,"name":"Mark Rehkämper","email":"","orcid":"","institution":"Imperial College London","correspondingAuthor":false,"prefix":"","firstName":"Mark","middleName":"","lastName":"Rehkämper","suffix":""}],"badges":[],"createdAt":"2025-06-13 12:38:21","currentVersionCode":1,"declarations":"","doi":"10.21203/rs.3.rs-6888308/v1","doiUrl":"https://doi.org/10.21203/rs.3.rs-6888308/v1","draftVersion":[],"editorialEvents":[{"content":"https://doi.org/10.1038/s41598-025-24419-4","type":"published","date":"2025-11-18T15:58:07+00:00"}],"editorialNote":"","failedWorkflow":false,"files":[{"id":84663193,"identity":"a5f67cc5-4968-4a97-ae4b-27fa0977f357","added_by":"auto","created_at":"2025-06-16 05:10:43","extension":"png","order_by":1,"title":"Figure 1","display":"","copyAsset":false,"role":"figure","size":45522,"visible":true,"origin":"","legend":"\u003cp\u003e\u003cstrong\u003eMass-independent Zn isotope compositions. \u003c/strong\u003eResults from the literature (SI) are presented as non-outlined markers. Results for Martian samples (BSM, outlined yellow diamonds) overlap with NCC values for ordinary (OC), enstatite (EC), and Rumuruti (R) chondrites, but are clearly distinct from carbonaceous chondrites (CC). Lunar samples (grey circles) display variable results.\u003c/p\u003e","description":"","filename":"1.png","url":"https://assets-eu.researchsquare.com/files/rs-6888308/v1/84158764f6e6986b5a87d382.png"},{"id":84663197,"identity":"f58a6c23-5928-46fa-a3bd-6fd3c7c67ab2","added_by":"auto","created_at":"2025-06-16 05:10:43","extension":"png","order_by":2,"title":"Figure 2","display":"","copyAsset":false,"role":"figure","size":37030,"visible":true,"origin":"","legend":"\u003cp\u003e\u003cstrong\u003eMass-independent Zn isotope composition of the Lunar samples.\u003c/strong\u003e e\u003csup\u003e66\u003c/sup\u003eZn and e\u003csup\u003e67\u003c/sup\u003eZn values for the five Lunar samples analysed in this study (grey) and BSE values (green) for comparison. The eZn values predicted for production in ECSNe (light grey field) and SN Ia (dark grey field) supernovae were modelled following Martins et al.\u003csup\u003e1\u003c/sup\u003e. The isotopic shifts from possible nuclear field shift effects (dashed black line) are also shown\u003csup\u003e1\u003c/sup\u003e.\u003c/p\u003e","description":"","filename":"2.png","url":"https://assets-eu.researchsquare.com/files/rs-6888308/v1/08f31cdc5969222a5a641139.png"},{"id":84663198,"identity":"28822abb-69b6-40d0-8f18-486acada127b","added_by":"auto","created_at":"2025-06-16 05:10:43","extension":"png","order_by":3,"title":"Figure 3","display":"","copyAsset":false,"role":"figure","size":68154,"visible":true,"origin":"","legend":"\u003cp\u003e\u003cstrong\u003eModelled Zn mass fractions derived from CC material for Mars and Earth.\u003c/strong\u003e (A) Probability density functions resulting from two Monte Carlo simulations that reproduce the nucleosynthetic Zn isotope compositions of BSM using all meteorite groups (yellow line) and only chondrites (dashed grey line). Most successful trials correspond to a CC Zn fraction of zero. (B) Same models as (A), but for the BSE. The most common combination that resulted in BSE-like compositions required ~36% and ~40% CC-like Zn, if only chondrites (green line) or all groups (dashed grey line) were employed, respectively.\u003c/p\u003e","description":"","filename":"3.png","url":"https://assets-eu.researchsquare.com/files/rs-6888308/v1/013532e0cbf5e3681362c0a6.png"},{"id":84663202,"identity":"53c100de-f67f-4e2f-a804-e26cd66cbaef","added_by":"auto","created_at":"2025-06-16 05:10:43","extension":"png","order_by":4,"title":"Figure 4","display":"","copyAsset":false,"role":"figure","size":176718,"visible":true,"origin":"","legend":"\u003cp\u003e\u003cstrong\u003eMixing models that attempt to reproduce the isotope and elemental composition of bulk Mars. \u003c/strong\u003eThe numbers on the panels correspond to the Run number of the simulation (Table 2). A) Mean mass fraction obtained for each meteorite group for all valid solutions (white lines) and respective uncertainties (2sd, coloured fields). The dashed lines illustrate the frequency at which each group appears in valid solutions, where f = 1 means that a given group appears in 100% of valid solutions. The CC fraction denotes the sum of all CC groups. B) Ratio of a given element to Al, normalized to CI chondrites. The lines represent the highest and lowest values obtained for all valid solutions, while the grey fields show estimates for Mars (Table S2). Elements shown with a solid line were used as criteria for the selection of valid results, while elements with dashed lines were not considered in the evaluation of results. C) Mean isotope compositions for all valid solutions of each run, with error bars indicating twice the standard deviation. Ratios shown with a solid line were used as criteria for selection of valid results, while ratios with a dashed line were not considered in the evaluation of results. The grey lines denote literature data for Mars (Table S1).\u003c/p\u003e","description":"","filename":"4.png","url":"https://assets-eu.researchsquare.com/files/rs-6888308/v1/8894983ab361ca8c47ea8a71.png"},{"id":96650326,"identity":"3c65bc1f-19f8-4acc-95b2-49d2e82757b7","added_by":"auto","created_at":"2025-11-24 16:11:09","extension":"pdf","order_by":0,"title":"","display":"","copyAsset":false,"role":"manuscript-pdf","size":1277437,"visible":true,"origin":"","legend":"","description":"","filename":"manuscript.pdf","url":"https://assets-eu.researchsquare.com/files/rs-6888308/v1/b7520e4c-20d5-4342-82d8-dbaccc35ced4.pdf"},{"id":84663196,"identity":"5db74182-1b69-4492-a789-6f69a9dee0be","added_by":"auto","created_at":"2025-06-16 05:10:43","extension":"docx","order_by":0,"title":"","display":"","copyAsset":false,"role":"supplement","size":115580,"visible":true,"origin":"","legend":"","description":"","filename":"SciRepMartianSI.docx","url":"https://assets-eu.researchsquare.com/files/rs-6888308/v1/30d73274749dc6467e7f7ac0.docx"},{"id":84663194,"identity":"abb9d8c0-43a4-41f9-b13c-f7f8d1bf09cd","added_by":"auto","created_at":"2025-06-16 05:10:43","extension":"xlsx","order_by":1,"title":"","display":"","copyAsset":false,"role":"supplement","size":19602,"visible":true,"origin":"","legend":"","description":"","filename":"SciRepcompilation.xlsx","url":"https://assets-eu.researchsquare.com/files/rs-6888308/v1/0854ede0873d055e7ec1cd7c.xlsx"}],"financialInterests":"No competing interests reported.","formattedTitle":"Provenance and distribution of zinc in terrestrial planets","fulltext":[{"header":"Introduction","content":"\u003cp\u003eConstraining the origins of volatiles in terrestrial planets is essential for understanding their formation and how they become habitable. Recent nucleosynthetic isotope studies showed that Earth\u0026rsquo;s inventories of the moderately volatile elements Zn and K are derived from mixed sources, including both NC planetesimals that formed locally as well as material akin to carbonaceous chondrites (CCs) that originated from much greater heliocentric distances\u003csup\u003e1-4\u003c/sup\u003e. Accretion of primitive material, which survived melting and differentiation in the early Solar System, has also been shown to play a crucial role in establishing Earth\u0026rsquo;s volatile content\u003csup\u003e5\u003c/sup\u003e. Nonetheless, it is unclear whether these features are common across terrestrial planets, or whether Earth presents a special case.\u003c/p\u003e\n\u003cp\u003eWhile Mars\u0026rsquo; Zn budget was supplied primarily by locally sourced NC material\u003csup\u003e6,7\u003c/sup\u003e, the contribution of primitive material to Martian volatiles remains unconstrained. Early work attempted to explain Mars\u0026rsquo; volatile content by mixing different nebular components with variable volatile abundances\u003csup\u003e8,9\u003c/sup\u003e. However, studies that reproduced the isotope composition of Mars by mixing of different chondritic endmembers typically resulted in bulk elemental compositions that were too volatile-rich\u003csup\u003e10-12\u003c/sup\u003e. Importantly, the extent of volatile depletion exhibited by a planet or planetesimal may not exclusively reflect nebular processes, as substantial volatile loss can occur during accretion. Heat derived from the decay of extinct radionuclides can produce enough energy to induce the formation of magma oceans in small, differentiated planetesimals, which allows for effective volatilization and degassing\u003csup\u003e13\u003c/sup\u003e. These processes furthermore produce mass-dependent isotope fractionations consistent with those observed in some planetesimals\u003csup\u003e14,15\u003c/sup\u003e. Therefore, planets accrete from a mixture of differentiated and undifferentiated materials, which likely shapes their volatile inventories.\u003c/p\u003e\n\u003cp\u003eAlbeit not directly, the composition and volatile content of a third terrestrial body can be investigated \u0026ndash; Theia, the Mars-sized planet that likely collided with proto-Earth to form the Moon\u003csup\u003e16\u003c/sup\u003e. Theia\u0026rsquo;s existence is inferred from the giant impact hypothesis \u0026ndash; the most prominent theory for the formation of the Moon\u003csup\u003e17,18\u003c/sup\u003e. This scenario calls for a collision between proto-Earth and Theia, leading to the formation of the Moon from the magma disk generated after impact. While the Moon is thought to have been primarily formed from the impactor, Theia\u0026rsquo;s composition remains elusive, as it cannot be directly accessed. Nonetheless, the similarities between the nucleosynthetic isotope compositions of the Earth and Moon\u003csup\u003e19-22\u003c/sup\u003e have been inferred to also extend to Theia. Due to their substantial volatile depletion, and considerable analytical challenges associated with measuring such limited samples, no nucleosynthetic isotope compositions of volatile elements are currently available for Lunar samples. The origin of volatiles for the Moon and Theia thus remain unconstrained.\u003c/p\u003e"},{"header":"Results","content":"\u003cp\u003eHere, we present mass-independent Zn isotope results for Martian and Lunar samples. The terrestrial rock reference material BCR-2, which was analysed concurrently for quality control, is indistinguishable in \u0026epsilon;Zn from the London Zn isotope standard (Table 1, Fig. 1). In contrast, all Martian meteorites display resolvable anomalies relative to the terrestrial composition, yielding results for bulk silicate Mars (BSM) in agreement with previous data\u003csup\u003e6,7\u003c/sup\u003e (i.e.,\u0026nbsp;e\u003csup\u003e66\u003c/sup\u003eZn\u003csub\u003eBSM\u003c/sub\u003e =\u0026nbsp;-0.15\u0026nbsp;\u0026plusmn;\u0026nbsp;0.04, 2se). Our accompanying results for the CI meteorite Orgueil are also consistent with previously published values for this meteorite (Table 1).\u003c/p\u003e\n\u003cp\u003eDue to the limited sample masses and their severe Zn depletion, the analyses of the Lunar samples used run solutions with Zn concentrations as low as 150 ng g\u003csup\u003e-1\u003c/sup\u003e (compared to up to 500 ng g\u003csup\u003e-1\u003c/sup\u003e for other samples), employed fewer data acquisition cycles, and encompassed fewer repeat runs than were obtained for other samples. This resulted in isotope data with larger uncertainties compared to the other results presented in this study (Table 1). The results for 15016-254 and 70017-587 are indistinguishable from terrestrial Zn and NC meteorites (e\u003csup\u003e66\u003c/sup\u003eZn =\u0026nbsp;-0.10\u0026nbsp;\u0026plusmn;\u0026nbsp;0.30 and\u0026nbsp;-0.11\u0026nbsp;\u0026plusmn;\u0026nbsp;0.07, respectively; Table 1, Fig. 2). In contrast,\u0026nbsp;NWA 11898 displays resolvable negative anomalies\u0026nbsp;relative to the terrestrial mean within \u0026plusmn;2se (e\u003csup\u003e66\u003c/sup\u003eZn =\u0026nbsp;-0.29\u0026nbsp;\u0026plusmn;\u0026nbsp;0.06), while NWA 11182 and 10017-423 display resolvable positive anomalies (i.e.:\u0026nbsp;e\u003csup\u003e67\u003c/sup\u003eZn = 0.40\u0026nbsp;\u0026plusmn;\u0026nbsp;0.11 and 0.44\u0026nbsp;\u0026plusmn;\u0026nbsp;0.21, respectively). \u0026nbsp;Finally, the mean obtained for the five Lunar samples (i.e.,\u0026nbsp;e\u003csup\u003e66\u003c/sup\u003eZn\u003csub\u003eLunar\u003c/sub\u003e = 0.01\u0026nbsp;\u0026plusmn;\u0026nbsp;0.19; 2se) overlaps with previously attained values for the BSE and NC chondrites\u003csup\u003e1\u003c/sup\u003e (NCCs; Fig. 1).\u003c/p\u003e"},{"header":"Discussion","content":"\u003cp\u003e\u003cstrong\u003eLunar samples\u003c/strong\u003e\u003c/p\u003e\n\u003cp\u003eLunar samples display identical mass-independent isotope compositions to the BSE for several isotope systems, such as O, W, Ca, Ti, and Cr\u003csup\u003e19-24\u003c/sup\u003e. Despite these similarities, dynamical models of the giant impact suggest that proto-Earth\u0026rsquo;s contribution to the Moon was limited, with approximately 70\u0026ndash;80% of the Lunar mass being derived from the giant impactor\u003csup\u003e16,25\u003c/sup\u003e. Combined, these observations may imply that the isotopic similarities also extended to Theia. However, the likelihood of an accretion scenario where Theia was isotopically identical to the BSE for most isotope systems is minimal, with one study estimating that there is less than a 1% chance for Theia and Earth to accrete with indistinguishable W and O isotope compositions\u003csup\u003e26\u003c/sup\u003e. \u003c/p\u003e\n\u003cp\u003eImportantly, the concentrations of non-volatile elements are very similar between CCs, NCCs, and differentiated meteorite parent bodies\u003csup\u003e27-31\u003c/sup\u003e. This contrasts with the distribution of volatile Zn, as this has highly variable abundances in different bodies, with concentrations ranging from less than 1 mg g\u003csup\u003e-1\u003c/sup\u003e in some meteorites from differentiated NC parent bodies (DNCs) to over 300 mg g\u003csup\u003e-1\u003c/sup\u003e in some CCs and NCCs\u003csup\u003e27-31\u003c/sup\u003e. Hence, even if Theia accreted from the same proportions of CCs, NCCs and DNCs as Earth, this could still result in a distinct nucleosynthetic Zn isotope composition, if the accreted materials differed in their Zn concentrations. In other words, two planets that share the same nucleosynthetic Zn isotope signature can only be generated if both the Zn isotope compositions and abundances of the accreting materials were essentially identical, and this constitutes a very unlikely scenario. An equally improbable explanation is that Theia and Earth accreted from different materials, which coincidently produced the same final bulk nucleosynthetic isotope composition. Hence, similar nucleosynthetic Zn isotope compositions for the Moon and the BSE would place even more significant constraints on the giant impact scenario. \u003c/p\u003e\n\u003cp\u003eThe improbability of a scenario where Theia was isotopically identical to the BSE led to the hypothesis of post-impact homogenization\u003csup\u003e26\u003c/sup\u003e. This scenario allows for distinct compositions for the impactor and the BSE, which would have been homogenized through vapor-phase equilibration between Earth\u0026rsquo;s mantle and the magma disk from which the Moon formed. Previous studies have shown that this scenario is feasible even for refractory elements, such as Ti\u003csup\u003e22\u003c/sup\u003e. Such a process should therefore inevitably affect Zn, which is volatile and, hence, more susceptible to vaporization and re-equilibration.\u003c/p\u003e\n\u003cp\u003eThe five Lunar samples display variable compositions, ranging from e\u003csup\u003e66\u003c/sup\u003eZn = -0.29 \u0026plusmn; 0.06 to e\u003csup\u003e66\u003c/sup\u003eZn = 0.29 \u0026plusmn; 0.39 (2se) (Fig.1, Table 1). All samples furthermore present a well-defined correlation between e\u003csup\u003e66\u003c/sup\u003eZn and e\u003csup\u003e67\u003c/sup\u003eZn values (R\u003csup\u003e2\u003c/sup\u003e = 0.98; Fig. 2). Importantly, the slope of this correlation is incompatible with variations predicted for nucleosynthetic isotope anomalies originating from either electron capture core collapse (ECSNe) or Type Ia (SN Ia) supernovae, which have been shown to be consistent with anomalies of other Solar System materials\u003csup\u003e1\u003c/sup\u003e (Fig. 2). It is hence likely that the observed variations reflect other processes that can affect mass-independent Zn isotope compositions.\u003c/p\u003e\n\u003cp\u003eResults of previous studies suggest that the mass-dependent Zn isotope compositions of Lunar samples were affected by kinetic isotope fractionation associated with evaporative Zn loss\u003csup\u003e32\u003c/sup\u003e. As such, it is possible that the exponential law, which was employed in the internal normalization procedure used here, did not adequately correct for the extent of kinetic mass-dependent isotopic fractionation experienced by some of the samples. The mass-dependent isotope compositions of the samples were thus calculated according to Eq. (S1). Importantly, these results were not obtained using the same method that was applied for the Martian samples (see SI) and are reported relative to the London Zn standard rather than JMC Lyon Zn standard. As such, the Lunar d\u003csup\u003e66\u003c/sup\u003eZn values are accompanied by larger uncertainties and may not exclusively reflect the natural composition of the samples, but also potentially isotope fractionation incurred during the analytical procedure. Nonetheless, they can be useful to assess whether any correlation between the extent of mass-dependent fractionation and the mass-independent results can be detected.\u003c/p\u003e\n\u003cp\u003eThe two samples with indistinguishable positive mass-independent isotope anomalies \u0026ndash; 10017-423 and NWA 11182 \u0026ndash; display clearly distinct mass-dependent isotope compositions, with mean d\u003csup\u003e66\u003c/sup\u003eZn values of -6.05\u0026permil; and 0.82\u0026permil;, respectively (Fig. S1). Similarly, the two samples that are indistinguishable from the BSE in e\u003csup\u003e66\u003c/sup\u003eZn (15016-254 and 70017-587) have markedly distinct mass-dependent isotope compositions (d\u003csup\u003e66\u003c/sup\u003eZn of -0.69\u0026permil; and 8.99\u0026permil;, respectively). Finally, the only sample that displays a negative e\u003csup\u003e66\u003c/sup\u003eZn anomaly (NWA 11898) is very fractionated (d\u003csup\u003e66\u003c/sup\u003eZn = 9.04\u0026permil;), with a mass-dependent isotope composition that that is comparable to that of 70017-587. Hence, the variability in mass-independent isotope composition does not appear to be influenced by mass-dependent isotope fractionation.\u003c/p\u003e\n\u003cp\u003eAll samples are derived from the Lunar surface, where they can be exposed to galactic cosmic rays, which could, in principle, alter Zn isotope compositions. Whilst still comparatively small, \u003csup\u003e67\u003c/sup\u003eZn has the largest neutron capture cross-section among the five Zn isotopes, and cosmogenic reactions could hence decrease the abundance of \u003csup\u003e67\u003c/sup\u003eZn through an induced (n,\u0026gamma;) reaction to produce \u003csup\u003e68\u003c/sup\u003eZn. The potential effects of this process can hence be most readily assessed by examining the e\u003csup\u003e67\u003c/sup\u003eZn values determined for the samples. Although sample 10017-423 displays the largest offset from the mean (e\u003csup\u003e67\u003c/sup\u003eZn = 0.44 \u0026plusmn; 0.21, 2se) and the highest cosmogenic exposure age (480 \u0026plusmn; 70 Ma)\u003csup\u003e33\u003c/sup\u003e, the positive e\u003csup\u003e67\u003c/sup\u003eZn value is the opposite of what would be expected for a decrease in the abundance of \u003csup\u003e67\u003c/sup\u003eZn caused by cosmogenic effects. Furthermore, the two other Apollo samples with identical e\u003csup\u003e67\u003c/sup\u003eZn values (e\u003csup\u003e67\u003c/sup\u003eZn = 0.03 \u0026plusmn; 0.07; e\u003csup\u003e67\u003c/sup\u003eZn = 0.02 \u0026plusmn; 0.16) have clearly distinct cosmogenic exposure ages (315 \u0026plusmn; 20 and 220 \u0026plusmn; 20 Ma, for 15016 and 70017, respectively)\u003csup\u003e34,35\u003c/sup\u003e (Fig. S1). Therefore, even if present, the effects of cosmogenic exposure on the mass-independent Zn isotope compositions of the analyzed samples are unlikely to be resolvable within the obtained precision.\u003c/p\u003e\n\u003cp\u003eSamples from the Lunar surface may also be contaminated by local impacting material that originates from isotopically distinct bodies. Previous studies found no substantial evidence for variations in the nucleosynthetic isotope composition of Lunar samples for other isotope systems\u003csup\u003e19-23\u003c/sup\u003e. However, Zn may be more susceptible to such alteration due to the severe Zn depletion recorded by the Moon. Nonetheless, as stated previously, the compositions of the Lunar samples define an excellent correlation, with a slope that is clearly distinct from the nucleosynthetic isotope variations predicted for the potential sources of the nucleosynthetic Zn anomalies (Fig. 2). The variability in the mass-independent Zn isotope composition of the Lunar samples is therefore unlikely to reflect contamination from isotopically distinct materials. Equally, the results are incompatible with modeled compositions for mass-independent isotope fractionation caused by the nuclear field shift effects (Fig. 2)\u003csup\u003e1\u003c/sup\u003e.\u003c/p\u003e\n\u003cp\u003eFinally, it is possible that the eZn data obtained for some samples are affected by isobaric or molecular interferences, or matrix effects. To test this, exploratory elemental analyses of sample solutions used for the Zn isotope analyses were performed using an iCAP Q inductively coupled plasma mass spectrometer (ICP-MS) at the University of Cambridge. Small aliquots of the three Apollo samples, Orgueil, and BCR-2 were taken after the Zn purification procedure. No systematic differences were detected between any of the samples, which display concentrations comparable to the blank for all fifty-seven elements that were analyzed. An aliquot of sample 10017-423 was furthermore subjected to a digestion protocol employing hydrogen peroxide in an attempt to eliminate organics possibly leached from the resins utilized in the ion exchange procedure\u003csup\u003e36\u003c/sup\u003e. This resulted in no detectable differences in the mass-independent isotope composition of this sample (e\u003csup\u003e66\u003c/sup\u003eZn = 0.58 \u0026plusmn; 0.18; e\u003csup\u003e67\u003c/sup\u003eZn = 0.53 \u0026plusmn; 0.10) from the mean obtained for aliquots that were not subjected to this procedure (e\u003csup\u003e66\u003c/sup\u003eZn = 0.22 \u0026plusmn; 0.46; e\u003csup\u003e67\u003c/sup\u003eZn = 0.42 \u0026plusmn; 0.26).\u003c/p\u003e\n\u003cp\u003eHence, while it is unclear which processes are recorded by the mass-independent Zn isotope composition of the Lunar samples in this study, it is unlikely that they all reflect the nucleosynthetic isotope composition of the Moon. As the only samples consistent with predicted nucleosynthetic isotope compositions, 15016-254 and 70017-587 are the least likely to have been affected by other processes and may in fact reflect the nucleosynthetic Zn isotope composition of the Moon. If so, this would define a mean nucleosynthetic Zn isotope composition for the Moon that is indistinguishable from the BSE (e\u003csup\u003e66\u003c/sup\u003eZn = -0.11 \u0026plusmn; 0.30; e\u003csup\u003e67\u003c/sup\u003eZn = 0.02 \u0026plusmn; 0.17), in line with findings for other isotope systems. However, with the available precision, the results are also indistinguishable from NCs (Fig. 1). Further analyses are hence required to confirm whether no distinctions can be resolved between the Lunar samples and the BSE.\u003c/p\u003e\n\u003cp\u003e\u003c/p\u003e\n\u003cp\u003e\u003cstrong\u003eMartian samples\u003c/strong\u003e\u003c/p\u003e\n\u003cp\u003eAs for non-volatile elements, the Martian samples analyzed in this study display resolvable nucleosynthetic Zn isotope anomalies relative to the BSE (e\u003csup\u003e66\u003c/sup\u003eZn\u003csub\u003eBSM\u003c/sub\u003e = -0.15 \u0026plusmn; 0.05; 2se), in line with previous studies\u003csup\u003e6,7\u003c/sup\u003e. The results for Mars furthermore overlap with data for NCCs\u003csup\u003e1,3,4\u003c/sup\u003e (Fig. 2). To estimate the CC contribution to Mars\u0026rsquo; Zn inventory, mixtures between different meteorite groups were modelled using a Monte Carlo simulation with 10,000 trials. In the first trial, all groups for which nucleosynthetic Zn isotope compositions are available were included (Supplementary Information). For each trial, the endmembers were randomly selected, and their compositions were generated in a normal distribution within the adopted values, along with arbitrary mass fractions between 0 and 100%. The final compositions of the mixtures were calculated by mass balance but only results which yielded Mars-like e\u003csup\u003e66\u003c/sup\u003eZn values were selected (e\u003csup\u003e66\u003c/sup\u003eZn\u003csub\u003eBSM\u003c/sub\u003e = -0.15 \u0026plusmn; 0.03, 2se; Table 1).\u003c/p\u003e\n\u003cp\u003eMost successful trials (63%) correspond to mixtures where no CCs were included, indicating that Mars\u0026rsquo; nucleosynthetic Zn isotope composition can be more readily reproduced by exclusively incorporating NC material (Fig. 3). The average CC-like Zn for all successful trials is ~16%, with 35% of them falling in the range ~1-20%. These results are in agreement with previous models which estimated a CC Zn contribution to Mars of ~23%\u003csup\u003e6\u003c/sup\u003e and up to ~22%\u003csup\u003e7\u003c/sup\u003e. However, differentiated materials have been estimated to have supplied just ~10% of Earth\u0026rsquo;s Zn\u003csup\u003e5\u003c/sup\u003e. Since their contribution is likely very limited, another run of the model was performed where only chondritic groups were included as endmembers. In this case, 43% of successful trials included no CCs, and 51% included between 1-20% CC-like Zn. As such, the inclusion of differentiated meteorite groups had only minor effects on the outcome of the model.\u003c/p\u003e\n\u003cp\u003eFor comparison, the same models were applied to the BSE (e\u003csup\u003e66\u003c/sup\u003eZn = -0.03 \u0026plusmn; 0.03, 2se). When all groups were included, trials with ~20-65% CC-like Zn were successful, with most results falling at ~40%, in line with previous studies\u003csup\u003e1,3,5,7\u003c/sup\u003e. In the run that employed only chondrites, most of the successful trials fall between ~15-55%, with maximum probability at ~36% CC material (Fig. 3). In either case, this defines a much more substantial CC contribution to the BSE than to BSM, since the latter appears to have received only a negligible Zn contribution from material with a CC origin.\u003c/p\u003e\n\u003cp\u003eIn addition to constraining the Zn contribution from CC materials, we also employed our results in a more comprehensive model to identify the main building blocks accreted by Mars. To do so, elemental concentrations were modelled for ten major elements (Na, Mg, Si, P, Ca, K, Ti, Fe, and Mn) and isotope compositions for nine isotope systems (\u0026Delta;\u003csup\u003e17\u003c/sup\u003eO, ɛ\u003csup\u003e48\u003c/sup\u003eCa, ɛ\u003csup\u003e50\u003c/sup\u003eTi, ɛ\u003csup\u003e54\u003c/sup\u003eCr, ɛ\u003csup\u003e64\u003c/sup\u003eZn, ɛ\u003csup\u003e84\u003c/sup\u003eSr, ɛ\u003csup\u003e96\u003c/sup\u003eZr, d\u003csup\u003e30\u003c/sup\u003eSi and d\u003csup\u003e25\u003c/sup\u003eMg) using the approach described in detail in Martins et al.\u003csup\u003e5\u003c/sup\u003e. The models employed Monte Carlo simulations with variable numbers of trials depending on the run (Table 2). To allow for a direct comparison with previously reported results for the BSE\u003csup\u003e5\u003c/sup\u003e, the same parameters and data were employed, including the use of ɛ\u003csup\u003e64\u003c/sup\u003eZn values internally normalized to the \u003csup\u003e66\u003c/sup\u003eZn/\u003csup\u003e67\u003c/sup\u003eZn ratio (Table S2). All relevant literature data for Mars summarized in Tables S3 and S4 (Supplementary information). The endmembers included CC (CI, CM, CV, CO) and NCC (H, L, LL ordinary chondrites and EH, EL enstatite chondrite) meteorite groups, as well as the parent bodies of two non-carbonaceous achondritic meteorites \u0026ndash; eucrites and angrites (EPB and APB, respectively), which are derived from differentiated non-carbonaceous (DNC) planetesimals.\u003c/p\u003e\n\u003cp\u003eThe endmembers were randomly selected and assigned arbitrary mass fractions for each of the trials. Their isotope and elemental compositions were randomly generated within the compiled literature values\u003csup\u003e5\u003c/sup\u003e. The resulting compositions of the mixtures were calculated by mass balance and the selection of valid results varied between runs. The mass fractions of each endmember and the resulting isotope compositions are reported as mean values and twice the standard deviation, based on all valid trials for each run. For the elemental abundances, the highest and lowest values obtained in valid runs are presented in Fig. 4. A total of four runs were performed, with each featuring distinct criteria for the selection of valid solutions (Table 2).\u003c/p\u003e\n\u003cp\u003eFor the first run of the model, only trials that yielded Mars-like mass-independent isotope compositions were selected (\u0026Delta;\u003csup\u003e17\u003c/sup\u003eO, ɛ\u003csup\u003e48\u003c/sup\u003eCa, ɛ\u003csup\u003e50\u003c/sup\u003eTi, ɛ\u003csup\u003e54\u003c/sup\u003eCr, ɛ\u003csup\u003e64\u003c/sup\u003eZn, ɛ\u003csup\u003e84\u003c/sup\u003eSr, and ɛ\u003csup\u003e96\u003c/sup\u003eZr), and this resulted in a mixture comprised mainly of NCCs (87 \u0026plusmn; 17%) with much more limited fractions of CCs (4 \u0026plusmn; 3%), and DNC material (13 \u0026plusmn; 11%). However, this produced elemental abundances that are inconsistent with literature estimates for Mars, with noticeable excesses of volatile elements (e.g., Na, P, K). The elemental abundances were successfully reproduced by Run 2, which produced a smaller NCC fraction (44 \u0026plusmn; 29%) combined with larger contributions from CCs (\u003cimg width=\"33\" height=\"16\" src=\"data:image/png;base64,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\" alt=\"image\"\u003e%) and DNCs (44 \u0026plusmn; 27%). The solutions resulting from this run, however, produced a wide range of mass-independent isotope compositions that were not compatible with literature values. Nonetheless, the mass-dependent d\u003csup\u003e30\u003c/sup\u003eSi and d\u003csup\u003e25\u003c/sup\u003eMg values of these mixtures were consistent with literature results for Mars.\u003c/p\u003e\n\u003cp\u003eFinally, no combination of these materials could reproduce both the Martian isotope compositions and the elemental abundances in Run 3. Combined, the results of Runs 1, 2, and 3 therefore imply that, in addition to CCs and NCCs, Mars likely accreted a significant fraction of DNC material that had NCC-like nucleosynthetic isotope compositions. One known DNC body was sampled by aubrites, a group of meteorites thought to originate from a differentiated enstatite chondrite-like planetesimal\u003csup\u003e37\u003c/sup\u003e. However, some of the data needed to characterize the endmember composition of this DNC meteorite group are unavailable\u003csup\u003e5\u003c/sup\u003e. Thus, in Run 4, hypothetical unsampled materials were adopted as DNC endmembers. In detail, these materials were characterized by the elemental abundances and mass-dependent isotope compositions of the APB and EPB, but the mass-independent isotope compositions of ordinary and enstatite chondrites, respectively, for Unsampled Materials 1 and 2 (UM1 and UM2). As such, UM1 and UM2 are equivalent to DNC enstatite and ordinary chondrite planetesimals, respectively\u003csup\u003e5\u003c/sup\u003e. With these parameters, Run 4 reproduced the isotope and elemental compositions of Mars with 53 \u0026plusmn; 23% of DNC, 47 \u0026plusmn; 23% of NCC, and 1 \u0026plusmn; 1% of CC material (Table 2, Fig. 4).\u003c/p\u003e\n\u003cp\u003eThe Run 4 results highlight a significant difference in the CC contributions to Earth (10 \u0026plusmn; 3%)\u003csup\u003e5\u003c/sup\u003e and Mars (1 \u0026plusmn; 1%) (Table 2, Fig. 4). Yet, the abundances of most volatile elements are higher for Mars than for Earth\u003csup\u003e38\u003c/sup\u003e. The results thus demonstrate that, while CCs may have played a substantial role in establishing Earth\u0026rsquo;s volatile inventory, material derived from a colder, volatile-rich region of the Solar System is not required to build a volatile-rich terrestrial planet. Instead, the more important determining factor appears to be the accretion of undifferentiated chondritic material, regardless of its origin within the Solar System. This chondritic material (NCC and CC combined) contributed ~30% and ~50% to the masses of Earth and Mars, respectively, but critically provided ~90% of the Zn inventories to both planets. The remaining accreting material was comprised of differentiated, volatile-poor planetesimals, which supplied just ~10% of the Zn.\u003c/p\u003e"},{"header":"Methods","content":"\u003cp\u003e\u003cstrong\u003eSamples and sample preparation\u003c/strong\u003e\u003c/p\u003e\n\u003cp\u003eThe study investigated three Apollo Lunar samples, two Lunar meteorites, and six Martian meteorites (Table 1). Digestion and preparation of the samples and the subsequent Zn isotope measurements were carried out in the MAGIC Laboratories at the Department of Earth Science \u0026amp; Engineering of Imperial College London, following the procedures outlined in Martins et al. \u003csup\u003e1\u003c/sup\u003e. All sample preparation was conducted in ISO Class 6 clean rooms, using ISO Class 4 laminar flow benches for critical steps. The water used was of \u0026ge; 18.2 M\u0026Omega; cm quality from a Millipore purification system. All acids were purified from reagent grade stock acids by sub-boiling distillation in either quartz glass (15.3 M HNO\u003csub\u003e3\u003c/sub\u003e, 6 M HCl) or Teflon (28 M HF, 12 M HCl, 8.5 M HBr) stills.\u003c/p\u003e\n\u003cp\u003eThe samples were completely crushed with an agate mortar and pestle and digested in Savillex Teflon beakers. The digestion procedure started with refluxing in a 2 + 1 mixture of 28 M HF + 15.3 M HNO\u003csub\u003e3\u003c/sub\u003e at 120 \u0026deg;C for at least two days on a hotplate, followed by evaporation to dryness. This process was then repeated with 6 M HCl. Following digestion, the samples were purified using the three-stage anion exchange procedure described in Martins et al.\u003csup\u003e1\u003c/sup\u003e.\u003c/p\u003e\n\u003cp\u003e\u003cstrong\u003eMass-independent Zn Isotope measurements\u003c/strong\u003e\u003c/p\u003e\n\u003cp\u003eThe isotope analyses were conducted with a Nu Instruments Nu Plasma II multiple collector inductively coupled plasma mass spectrometer (MC-ICP-MS). A Nu Instruments DSN 100 desolvation system fitted with glass cross flow nebulizers with solution flow rates of about 120 \u0026mu;l min\u003csup\u003e-1\u003c/sup\u003e were employed for sample introduction in conjunction with a CETAC ASX 112FR autosampler. The analytical procedures followed the methods described in Martins et al. \u003csup\u003e5\u003c/sup\u003e.\u003c/p\u003e\n\u003cp\u003eMost samples were analysed using two cup configuration\u003csup\u003e1\u003c/sup\u003e. However, samples with limited Zn were occasionally analysed using a single cup configuration and without performing a correction for Ge interferences on \u003csup\u003e70\u003c/sup\u003eZn\u003csup\u003e5\u003c/sup\u003e. All ion beams were monitored using Faraday cups fitted with 10\u003csup\u003e11\u003c/sup\u003e \u0026Omega; resistors. Each run was started by a peak centering routine, whilst each block commenced with a 60 s measurement of the electronic baselines of the Faraday collectors whilst the ion beam was deflected in the electrostatic analyser. Data acquisition for the Martian samples encompassed 3 blocks with 20 measurement cycles of 8 s each. Due to the low Zn contents of the Lunar samples, their analyses encompassed only 2 blocks with 20 data acquisition cycles.\u003c/p\u003e\n\u003cp\u003eThe samples were introduced as solutions in 0.1 M HNO\u003csub\u003e3\u003c/sub\u003e, typically containing 150-500 ng g\u003csup\u003e-1\u003c/sup\u003e of Zn, with instrumental sensitivity ranging between 150 and 350 V (\u0026micro;g ml\u003csup\u003e-1\u003c/sup\u003e)\u003csup\u003e-1\u003c/sup\u003e. All sample analyses were carried out with the sample\u0026ndash;standard bracketing technique, in which sample runs were symmetrically bracketed by runs of the London Zn isotope reference material. The Zn concentrations of the latter were matched to the sample concentrations to within 10 to 15%.\u003c/p\u003e\n\u003cp\u003eThe Zn isotope results are reported using the \u0026epsilon; notation, which denotes deviations of the measured isotope ratio for a sample (sam) from the value determined for the London Zn reference standard (std) in parts per 10\u003csup\u003e4\u003c/sup\u003e:\u003c/p\u003e\n\u003cp\u003e\u003cimg 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width=\"337\" height=\"69\"\u003e\u003c/p\u003e\n\u003cp\u003ewhere i/68 is the isotope ratio of interest and the \u003csup\u003e64\u003c/sup\u003eZn/\u003csup\u003e68\u003c/sup\u003eZn ratio that was used for internal normalization with the exponential law. Additional results obtained using \u003csup\u003e66\u003c/sup\u003eZn/\u003csup\u003e67\u003c/sup\u003eZn for internal normalization are reported in the Supplementary Information (Table S2).\u003c/p\u003e"},{"header":"Declarations","content":"\u003cp\u003e\u003cstrong\u003eAcknowledgements\u003c/strong\u003e\u003c/p\u003e\n\u003cp\u003eWe are grateful to the NASA Johnson Space Center (R. Zeigler) for providing the Apollo samples, and the Natural History Museum London for the Orgueil sample. The US Antarctic meteorite samples are from the Antarctic Search for Meteorites (ANSMET) program; they are curated by the Dept. of Mineral Sciences of the Smithsonian Institution and the Astromaterials Curation Office at NASA Johnson Space Center. We also thank Jason Day and Helena Pryer for their assistance in the laboratory. This work was funded by an Imperial College London President\u0026rsquo;s PhD Scholarship (R.M.), an ERC Advanced grant 101020665 (R.M., H.M.W.), an UKRI STFC grant ST/W001179/1 (M.R., E.M.M.).\u003c/p\u003e\n\u003cp\u003e\u003cstrong\u003eAuthor contributions\u003c/strong\u003e\u003c/p\u003e\n\u003cp\u003eM.R. designed the research. R.M., E.M.M. and Y.H. performed the sample preparation and analyses. R.M. performed the modeling. All authors contributed to interpretation. R.M. wrote the first draft of the manuscript, which was subsequently edited by all authors.\u003c/p\u003e\n\u003cp\u003e\u003cstrong\u003eCompeting interests\u003c/strong\u003e\u003c/p\u003e\n\u003cp\u003eThe author(s) declare no competing interests.\u003c/p\u003e\n\u003cp\u003e\u003cstrong\u003eData availability\u003c/strong\u003e\u003c/p\u003e\n\u003cp\u003eAll data generated or analysed during this study are included in this published article (and its supplementary information files).\u003c/p\u003e"},{"header":"References","content":"\u003col\u003e\n\u003cli\u003eMartins, R., Kuthning, S., Coles, B. J., Kreissig, K. \u0026amp; Rehk\u0026auml;mper, M. Nucleosynthetic isotope anomalies of zinc in meteorites constrain the origin of Earth\u0026rsquo;s volatiles. \u003cem\u003eScience\u003c/em\u003e \u003cstrong\u003e379\u003c/strong\u003e, 369-372 (2023).\u003c/li\u003e\n\u003cli\u003eNie, N. 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Astron.\u003c/em\u003e \u003cstrong\u003e7\u003c/strong\u003e, 182-189 (2023).\u003c/li\u003e\n\u003cli\u003eFang, L.\u003cem\u003e et al.\u003c/em\u003e The origin of 4-Vesta\u0026rsquo;s volatile depletion revealed by the zinc isotopic composition of diogenites. \u003cem\u003eSci. Adv.\u003c/em\u003e \u003cstrong\u003e10\u003c/strong\u003e, eadl1007 (2024).\u003c/li\u003e\n\u003c/ol\u003e"},{"header":"Tables","content":"\u003cp\u003e\u003cstrong\u003eTable 1. Mass-independent Zn isotope data (in \u0026epsilon;Zn notation) for meteorite, Martian, Lunar and terrestrial samples.\u0026nbsp;\u003c/strong\u003e\u003c/p\u003e\n\u003ctable border=\"0\" cellspacing=\"0\" cellpadding=\"0\"\u003e\n \u003ctbody\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003e\u003cstrong\u003eSample name\u003c/strong\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003e\u003cstrong\u003eType\u003c/strong\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e\u003cstrong\u003eMass (g)\u003c/strong\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e\u003cstrong\u003ee\u003c/strong\u003e\u003cstrong\u003e\u003csup\u003e66\u003c/sup\u003e\u003c/strong\u003e\u003cstrong\u003eZn\u003c/strong\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e\u003cstrong\u003e2sd\u003c/strong\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e\u003cstrong\u003e2se\u003c/strong\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e\u003cstrong\u003ee\u003c/strong\u003e\u003cstrong\u003e\u003csup\u003e67\u003c/sup\u003e\u003c/strong\u003e\u003cstrong\u003eZn\u003c/strong\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e\u003cstrong\u003e2sd\u003c/strong\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e\u003cstrong\u003e2se\u003c/strong\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e\u003cstrong\u003en\u003c/strong\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003eMIL 03346\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eNakhlite\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e0.310\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.26\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.32\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.12\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.05\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.32\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.12\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e7\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003eALH 77005\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eShergottite\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e0.290\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.10\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.26\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.09\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.04\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.42\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.15\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e8\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003eEET 79001\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eShergottite\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e0.300\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.20\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.23\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.09\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.03\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.39\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.16\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e6\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003eLAR 12095\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eShergottite\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e0.300\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.08\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.21\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.07\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.16\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.21\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.08\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e7\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003eRBT 04262\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eShergottite\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e0.300\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.14\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.18\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.07\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.06\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.22\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.09\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e6\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003eALH 84001\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eSNC OPX\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e0.300\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.12\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.23\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.07\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.10\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.32\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.09\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e12\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003e\u003cem\u003eBSM\u003c/em\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.15\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.12\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.05\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.06\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.12\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.05\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e6\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003e70017-587\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eHigh-Ti Mare Basalt\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e1.898\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.11\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.21\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.07\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.03\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.22\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.07\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e9\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003e10017-423\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eHigh-Ti Ilmenite Basalt\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e0.400\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.29\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.87\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.39\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.44\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.48\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.21\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e5\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003e15016-254\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eLow-Ti Olivine Basalt\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e2.400\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.10\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e-\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.30\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.02\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e-\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.17\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e2\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003eNWA 11182\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eFeldspathic breccia\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e2.000\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.18\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e-\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.19\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.40\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e-\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.11\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e2\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003eNWA 11898\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eFeldspathic breccia\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\n \u003cp\u003e2.050\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.29\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.13\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.06\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.17\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.08\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.04\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e4\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003e\u003cem\u003eLunar mean\u003c/em\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.01\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.43\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.19\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.14\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.48\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.21\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e5\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003eOrgueil\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eCI\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.32\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.24\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.06\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e-0.07\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.25\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.06\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e18\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 16.7496%;\"\u003e\n \u003cp\u003eBCR-2\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 25.7048%;\"\u003e\n \u003cp\u003eTerrestrial\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 10.9453%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.00\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.26\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.04\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 7.79436%;\"\u003e\n \u003cp\u003e0.00\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.27\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 6.30182%;\"\u003e\n \u003cp\u003e0.05\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 5.80431%;\"\u003e\n \u003cp\u003e34\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003c/tbody\u003e\n\u003c/table\u003e\n\u003cp\u003en is the total number of individual analytical runs for a given meteorite, for one or several powder/digest solution aliquots.\u003c/p\u003e\n\u003cp\u003e\u003cstrong\u003eTable 2. Summary of results from the Monte Carlo simulations for the building blocks of Mars.\u003c/strong\u003e\u003c/p\u003e\n\u003ctable border=\"0\" cellspacing=\"0\" cellpadding=\"0\" width=\"100%\"\u003e\n \u003ctbody\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 32.3232%;\"\u003e\n \u003cp\u003eRun\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e1\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e2\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e3\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 13.1313%;\"\u003e\n \u003cp\u003e4\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 32.3232%;\"\u003e\n \u003cp\u003eNucleosynthetic isotope composition\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e✓\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e✓\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 13.1313%;\"\u003e\n \u003cp\u003e✓\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 32.3232%;\"\u003e\n \u003cp\u003eMajor elements ratios\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\u003cbr\u003e\u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e✓\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e✓\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 13.1313%;\"\u003e\n \u003cp\u003e✓\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 32.3232%;\"\u003e\n \u003cp\u003eEndmembers\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003eCC, NCC, APB, EPB\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003eCC, NCC, APB, EPB\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003eCC, NCC, APB, EPB\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 13.1313%;\"\u003e\n \u003cp\u003eCC, NCC, UM1, UM2\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 32.3232%;\"\u003e\n \u003cp\u003eTrials\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e10\u003csup\u003e8\u003c/sup\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e10\u003csup\u003e4\u003c/sup\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e10\u003csup\u003e8\u003c/sup\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 13.1313%;\"\u003e\n \u003cp\u003e10\u003csup\u003e8\u003c/sup\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 32.3232%;\"\u003e\n \u003cp\u003eSolutions\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e478\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e2428\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e0\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 13.1313%;\"\u003e\n \u003cp\u003e787\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 32.3232%;\"\u003e\n \u003cp\u003eCC (%,\u0026nbsp;\u0026plusmn;\u0026nbsp;2sd)\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e4\u0026nbsp;\u0026plusmn;\u0026nbsp;3\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e\u003cimg width=\"36\" height=\"16\" src=\"data:image/png;base64,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\" alt=\"image\"\u003e\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e-\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 13.1313%;\"\u003e\n \u003cp\u003e1\u0026nbsp;\u0026plusmn;\u0026nbsp;1\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 32.3232%;\"\u003e\n \u003cp\u003eNCC (%,\u0026nbsp;\u0026plusmn;\u0026nbsp;2sd)\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e87\u0026nbsp;\u0026plusmn;\u0026nbsp;17\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e44\u0026nbsp;\u0026plusmn;\u0026nbsp;29\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e-\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 13.1313%;\"\u003e\n \u003cp\u003e47\u0026nbsp;\u0026plusmn;\u0026nbsp;23\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003ctr\u003e\n \u003ctd style=\"width: 32.3232%;\"\u003e\n \u003cp\u003eAPB/EPB/UM (%,\u0026nbsp;\u0026plusmn;\u0026nbsp;2sd)\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e13\u0026nbsp;\u0026plusmn;\u0026nbsp;11\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e44\u0026nbsp;\u0026plusmn;\u0026nbsp;27\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 18.1818%;\"\u003e\n \u003cp\u003e-\u003c/p\u003e\n \u003c/td\u003e\n \u003ctd style=\"width: 13.1313%;\"\u003e\n \u003cp\u003e53\u0026nbsp;\u0026plusmn;\u0026nbsp;23\u003c/p\u003e\n \u003c/td\u003e\n \u003c/tr\u003e\n \u003c/tbody\u003e\n\u003c/table\u003e\n\u003cp\u003eCheckmarks indicate literature values for Mars that are successfully reproduced by each run. Meteorite groups included in the models: CI, CM, CO, CV, EH, EL, H, L, LL, eucrite parent body (EPB), angrite parent body (APB), and Unsampled Materials 1 and 2, UM1 and UM2. UM1 and UM2 have eucrite- and angrite-like elemental abundances and mass-dependent isotope compositions, but OC and EC-like nucleosynthetic isotope compositions, respectively, following Martins et al.\u003csup\u003e5\u003c/sup\u003e.\u003c/p\u003e"}],"fulltextSource":"","fullText":"","funders":[],"hasAdminPriorityOnWorkflow":false,"hasManuscriptDocX":true,"hasOptedInToPreprint":true,"hasPassedJournalQc":"","hasAnyPriority":true,"hideJournal":false,"highlight":"","institution":"","isAcceptedByJournal":true,"isAuthorSuppliedPdf":false,"isDeskRejected":"","isHiddenFromSearch":false,"isInQc":false,"isInWorkflow":false,"isPdf":false,"isPdfUpToDate":true,"isWithdrawnOrRetracted":false,"journal":{"display":true,"email":"[email protected]","identity":"scientific-reports","isNatureJournal":false,"hasQc":true,"allowDirectSubmit":false,"externalIdentity":"scirep","sideBox":"Learn more about [Scientific Reports](http://www.nature.com/srep/)","snPcode":"","submissionUrl":"","title":"Scientific Reports","twitterHandle":"","acdcEnabled":true,"dfaEnabled":true,"editorialSystem":"stoa","reportingPortfolio":"Scientific Reports","inReviewEnabled":true,"inReviewRevisionsEnabled":true},"keywords":"","lastPublishedDoi":"10.21203/rs.3.rs-6888308/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-6888308/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"Analyses of Earth’s nucleosynthetic Zn isotope composition indicate that its inventory of this volatile element was derived from a mixture of materials originating in both the inner and outer regions of the Solar System. In contrast, the nucleosynthetic Zn isotope composition of Martian meteorites suggests that, despite being more volatile-rich than Earth, Mars received very limited Zn from outer Solar System sources. Modeling for Earth also indicates that, although only ~30% of its mass was supplied by chondritic material, such undifferentiated, primitive bodies contributed ~90% of its Zn. However, the total chondritic contribution to Mars, and its role in shaping the planet’s volatile budget, remain poorly constrained. Here, we present nucleosynthetic Zn isotope data for six Martian meteorites, confirming that Mars’ Zn was likely sourced exclusively from inner Solar System material. These data were incorporated into a comprehensive mixing model that includes constraints from eight additional isotope systems and major element abundances. The results are consistent with Mars having accreted ~50% of its mass from chondritic material, which also delivered ~90% of its Zn. Together, these findings suggest that the proportion of undifferentiated material accreted by a planet plays a more critical role in establishing its volatile budget than the specific provenance of the accreting sources. Finally, we report mass-independent Zn isotope compositions for five Lunar samples. The results are indistinguishable, within uncertainty, from values for the bulk silicate Earth (BSE) and non-carbonaceous (NC) meteorites. Further analyses are thus required to reliably constrain the origin of Lunar Zn.","manuscriptTitle":"Provenance and distribution of zinc in terrestrial planets","msid":"","msnumber":"","nonDraftVersions":[{"code":1,"date":"2025-06-16 05:10:38","doi":"10.21203/rs.3.rs-6888308/v1","editorialEvents":[{"type":"communityComments","content":1},{"type":"decision","content":"Revision requested","date":"2025-07-09T18:39:12+00:00","index":"","fulltext":""},{"type":"editorInvitedReview","content":"","date":"2025-07-04T14:24:00+00:00","index":"hide","fulltext":""},{"type":"editorInvitedReview","content":"","date":"2025-07-02T14:13:13+00:00","index":"hide","fulltext":""},{"type":"reviewerAgreed","content":"283178926433942674232479876213794569428","date":"2025-06-18T14:25:57+00:00","index":"hide","fulltext":""},{"type":"reviewerAgreed","content":"318940484655162970944453191081198614727","date":"2025-06-18T06:49:15+00:00","index":"hide","fulltext":""},{"type":"reviewerAgreed","content":"220120362507515563658173292407150184463","date":"2025-06-16T16:40:38+00:00","index":"hide","fulltext":""},{"type":"reviewersInvited","content":"","date":"2025-06-16T16:03:27+00:00","index":"","fulltext":""},{"type":"editorAssigned","content":"","date":"2025-06-16T16:00:20+00:00","index":"","fulltext":""},{"type":"editorInvited","content":"","date":"2025-06-16T07:05:40+00:00","index":"","fulltext":""},{"type":"checksComplete","content":"","date":"2025-06-14T04:29:32+00:00","index":"","fulltext":""},{"type":"submitted","content":"Scientific Reports","date":"2025-06-13T12:31:19+00:00","index":"","fulltext":""}],"status":"published","journal":{"display":true,"email":"[email protected]","identity":"scientific-reports","isNatureJournal":false,"hasQc":true,"allowDirectSubmit":false,"externalIdentity":"scirep","sideBox":"Learn more about [Scientific Reports](http://www.nature.com/srep/)","snPcode":"","submissionUrl":"","title":"Scientific Reports","twitterHandle":"","acdcEnabled":true,"dfaEnabled":true,"editorialSystem":"stoa","reportingPortfolio":"Scientific Reports","inReviewEnabled":true,"inReviewRevisionsEnabled":true}}],"origin":"","ownerIdentity":"d0d8e18d-8f77-4fda-853c-c63e6d4c2bc9","owner":[],"postedDate":"June 16th, 2025","published":true,"recentEditorialEvents":[],"rejectedJournal":[],"revision":"","amendment":"","status":"published-in-journal","subjectAreas":[{"id":50038129,"name":"Earth and environmental sciences/Planetary science/Early solar system"},{"id":50038130,"name":"Physical sciences/Astronomy and planetary science/Planetary science/Inner planets"}],"tags":[],"updatedAt":"2025-11-24T16:06:21+00:00","versionOfRecord":{"articleIdentity":"rs-6888308","link":"https://doi.org/10.1038/s41598-025-24419-4","journal":{"identity":"scientific-reports","isVorOnly":false,"title":"Scientific Reports"},"publishedOn":"2025-11-18 15:58:07","publishedOnDateReadable":"November 18th, 2025"},"versionCreatedAt":"2025-06-16 05:10:38","video":"","vorDoi":"10.1038/s41598-025-24419-4","vorDoiUrl":"https://doi.org/10.1038/s41598-025-24419-4","workflowStages":[]},"version":"v1","identity":"rs-6888308","journalConfig":"researchsquare"},"__N_SSP":true},"page":"/article/[identity]/[[...version]]","query":{"redirect":"/article/rs-6888308","identity":"rs-6888308","version":["v1"]},"buildId":"8U1c8b4HqxoKbykW_rLl7","isFallback":false,"isExperimentalCompile":false,"dynamicIds":[84888],"gssp":true,"scriptLoader":[]}