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Tracing the Origins of the Ice Giants Through Noble Gas Isotopic Composition

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Abstract

The current composition of giant planet atmospheres provides information on how such planets formed, and on the origin of the solid building blocks that contributed to their formation. Noble gas abundances and their isotope ratios are among the most valuable pieces of evidence for tracing the origin of the materials from which the giant planets formed. In this review we first outline the current state of knowledge for heavy element abundances in the giant planets and explain what is currently understood about the reservoirs of icy building blocks that could have contributed to the formation of the Ice Giants. We then outline how noble gas isotope ratios have provided details on the original sources of noble gases in various materials throughout the solar system. We follow this with a discussion on how noble gases are trapped in ice and rock that later became the building blocks for the giant planets and how the heavy element abundances could have been locally enriched in the protosolar nebula. We then provide a review of the current state of knowledge of noble gas abundances and isotope ratios in various solar system reservoirs, and discuss measurements needed to understand the origin of the ice giants. Finally, we outline how formation and interior evolution will influence the noble gas abundances and isotope ratios observed in the ice giants today. Measurements that a future atmospheric probe will need to make include (1) the 3He/4He isotope ratio to help constrain the protosolar D/H and 3He/4He; (2) the 20Ne/22Ne and 21Ne/22Ne to separate primordial noble gas reservoirs similar to the approach used in studying meteorites; (3) the Kr/Ar and Xe/Ar to determine if the building blocks were Jupiter-like or similar to 67P/C-G and Chondrites; (4) the krypton isotope ratios for the first giant planet observations of these isotopes; and (5) the xenon isotopes for comparison with the wide range of values represented by solar system reservoirs.

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Abbreviations

67P/C-G:

67P/Churyumov-Gerasimenko

ACTZ:

amorphous-to-crystalline transition zone

AGB:

Asymptotic Giant Branch

BB:

Building Blocks

BB1:

Building blocks that form the core of a giant planet during core accretion

BB2:

Building blocks that are accreted during stages two and three of core accretion

BB3:

Impactors that add to the heavy elements in the envelope after a giant planet has formed

GPMS:

Galileo Probe Mass Spectrometer

HL:

H for heavy, r-process isotopes, L for light, p-process isotopes

IDP:

Interplanetary Dust Particles

ISM:

Interstellar Medium

PSN:

Protosolar Nebula

SiC:

Silicon Carbide

SW:

Solar wind

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Acknowledgements

K.E.M. acknowledges support from the Rosetta project through JPL subcontract 1585002, by NFDAP grant 80NSSC18K1233, and by RDAP grant 80NSSC19K1306. O.M. and B.M. acknowledge support from CNES. JIL acknowledges support from the Juno mission through Subcontract D99069MO from the Southwest Research Institute.

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Authors and Affiliations

  1. Johns Hopkins University Applied Physics Laboratory, Laurel, MD, 240-592-0262, USA

    K. E. Mandt & A. Luspay-Kuti

  2. Aix Marseille Université, CNRS, CNES, LAM (Laboratoire d’Astrophysique de Marseille), UMR 7326, 13388, Marseille, France

    O. Mousis & A. Aguichine

  3. Department of Astronomy and Carl Sagan Institute, Cornell University, Ithaca, NY, 14853, USA

    J. Lunine

  4. Centre de Recherches Pétrographiques et Géochimiques, UMR 7358, CNRS & Université de Lorraine, Vandoeuvre-lès-Nancy, France

    B. Marty

  5. Chinese Academy of Sciences, Beijing, China

    T. Smith

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  1. K. E. Mandt
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In Situ Exploration of the Ice Giants: Science and Technology

Edited by Olivier J. Mousis and David H. Atkinson

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Mandt, K.E., Mousis, O., Lunine, J. et al. Tracing the Origins of the Ice Giants Through Noble Gas Isotopic Composition. Space Sci Rev 216, 99 (2020). https://doi.org/10.1007/s11214-020-00723-5

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