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The NC-CC Isotope Dichotomy: Implications for the Chemical and Isotopic Evolution of the Early Solar System

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Abstract

Understanding the formation of our planetary system requires identification of the materials from which it originated and the accretion processes that produced the planets. The compositional evolution of the solar system can be constrained by synthesizing astronomical datasets and numerical models with elemental and isotopic compositions from objects that directly sampled the disk: meteorites and their constituents (chondrules, refractory inclusions, and matrix). This contribution reviews constraints on early solar system evolution provided by the so-called non-carbonaceous (NC) and carbonaceous chondrite (CC) groups and their relationship to the volatile element characteristics of chondritic meteorites. In previous work, the NC or CC character of a parent body was used to infer its accretion location in the protoplanetary disk. The NC groups purportedly originated in the inner disk, and the CC groups were derived from the outer disk, where the NC and CC regions of the disk may have been separated early on by proto-Jupiter, a pressure maximum, or a dust trap in the disk. The tenet that all CC parent bodies accreted in the outer disk is, in part, based on evidence that a handful of CC meteorites are enriched in volatile species compared to NC meteorites. Here, it is reviewed if and how the volatile element and nucleosynthetic isotope compositions of meteorites can be linked to accretion locations within the disk. The nucleosynthetic isotope compositions of whole rock meteorite samples contrast the trends found for their major volatile element compositions (i.e., C, N, and O). Although there may be an increase in volatile abundances when comparing some stony NC and CC meteorites and their inferred accretion locations within the disk, this is not necessarily a general rule. The difficulties with inferring parent body accretion locations are discussed. It is found that it cannot always be assumed that parent bodies which formed in the CC reservoir are “volatile-rich” relative to those that formed in the NC reservoir which are “volatile-poor”. Consequently, tracing the origin of terrestrial volatiles using the NC-CC isotope dichotomy remains challenging.

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Notes

  1. The IUPAC-IUGS convention for expressing dates following recommendation by Holden et al. (2011) is that annus (a) is used for one year as a unit of time, both for absolute time and time differences. Hence, considering the declensions, it is Ga = Giga annis (ablative for age; used as appellative) or Ga = Giga annos (pl. accusative, for how long ago).

  2. The enrichments of C, N, and O (relative to solar) observed in outer planet atmospheres were caused by the accretion of ices bearing these highly volatile elements. Highly volatile elements have 50% condensation temperatures below 371 K, volatile elements below 665 K, moderately volatiles between 1335 and 665 K, and refractories above 1335 K (for a gas of solar composition at a total pressure of 10−4 bar; Lodders 2003). See last chapter in this edition by K. Lodders for elemental data for the Sun and meteorites.

  3. Typically, isotope ratios are measured, and meteorite samples with an excess or depletion of a given isotope will have a higher or lower (respectively) isotope ratio than the terrestrial reference value. Positive or negative isotope anomalies arise from the definition of the isotope notation, which is the difference between the measured sample ratio from that of the terrestrial standard value in percent (%), permil (‰), on a scale of parts per 10,000 (\(\varepsilon \) units), or in parts per 1,000,000 (\(\mu \) units). The advantage of using the differences in the ratios is that these scales are easier to work with, especially for samples with small isotope anomalies (bulk meteorites, chondrules, CAIs). Terrestrial materials are generally defined as ‘normal’ (or equal to zero) in isotopic composition.

  4. Additional sources of achondrites to Earth include Mars and the Moon. The meteorites referred to here do not include micrometeorites.

  5. Proposals for the origin of meteoritic oxygen isotopic variations now include photochemical effects (Clayton 2002) and non-mass dependent isotopic effects (Thiemens and Heidenreich 1983).

  6. Measurable retention of any originally accreted water (ice) on the parent body requires post-accretion aqueous alteration; the water abundance then also depends on kinetics and the degree of aqueous processing and/or thermal metamorphism on the parent body. It should be noted that important intra- and inter-chondrite variations in water concentrations exist which can be explained, in part, by varying proportions of H-bearing components in a given (sub-)sample (e.g., Pearson et al. 2001). Analytically, not all extraction techniques may clearly distinguish between primordial and (terrestrial) adsorbed water (e.g., Robert and Epstein 1982; Vacher et al. 2020), and terrestrial exposure of “finds” can modify water concentrations (Stephant et al. 2018). Thus, the reported bulk water contents of chondrites cannot directly reflect the original accreted water in all cases.

  7. Individual CI and CM chondrites record a wide range of hydrogen isotope (\(\delta \)D) values, possibly due, in part, to variable degrees of aqueous alteration and sampling biases (Alexander et al. 2012, 2018; Kerridge 1985; Robert 2003). Therefore, Alexander et al. (2018) used average values of 78 ± 7‰ and –53 ± 130‰ for the CI and CM chondrite groups, respectively.

  8. The different chondrite groups (e.g., CI, CM, CR, CO, CV, CK) within a given class (e.g., carbonaceous chondrites) record a wide range of \(\delta ^{15}\)N values (e.g., Pearson et al. 2006). For a given group, the \(\delta ^{15}\)N value varies with petrologic type, i.e., the extent of thermal metamorphism; \(\delta ^{15}\)N generally decreases with increasing petrologic type from 1 to 4 (Pearson et al. 2006). In addition, the nitrogen extraction method (combustion \(\mathit{vs}\). pyrolysis) can yield distinct \(\delta ^{15}\)N values (e.g., Grady et al. 1986). Therefore, care should be taken when comparing data from different studies.

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Acknowledgements

We thank the International Space Science Institute (Bern, CH) for hosting and supporting the workshop “Reading Terrestrial Planet Evolution in Isotopes and Element Measurements” and the editors of this book. Our sincere thanks to editor in chief H. Lammer for his guidance and patience. We also thank thorough reviews by A.M. Davis and C.M.O’D. Alexander. KRB was supported by NASA Emerging Worlds grants 80NSSC18K0496 and NNX16AN07G, NASA SSERVI grant NNA14AB07A, and the Department of Earth and Planetary Sciences, Rutgers University. EF and BM were supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreements no. 715028 and no. 695618, respectively). Work by KL was supported in part by NSF grant AST 1517541 and the McDonnell Centre for the Space Sciences. This is CRPG-CNRS contribution 2374.

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Authors and Affiliations

  1. Department of Earth and Planetary Sciences, Rutgers University, Piscataway, NJ, 08854, USA

    Katherine R. Bermingham

  2. Department of Geology, University of Maryland, College Park, MD, 20742, USA

    Katherine R. Bermingham

  3. Université de Lorraine, CNRS, CRPG, 54000, Nancy, France

    Evelyn Füri & Bernard Marty

  4. Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, Washington University in St. Louis, St. Louis, MO, 63130, USA

    Katharina Lodders

Authors
  1. Katherine R. Bermingham
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  2. Evelyn Füri
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  3. Katharina Lodders
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  4. Bernard Marty
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Reading Terrestrial Planet Evolution in Isotopes and Element Measurements

Edited by Helmut Lammer, Bernard Marty, Aubrey L. Zerkle, Michel Blanc, Hugh O’Neill and Thorsten Kleine

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Bermingham, K.R., Füri, E., Lodders, K. et al. The NC-CC Isotope Dichotomy: Implications for the Chemical and Isotopic Evolution of the Early Solar System. Space Sci Rev 216, 133 (2020). https://doi.org/10.1007/s11214-020-00748-w

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  • DOI: https://doi.org/10.1007/s11214-020-00748-w

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