Bifurcation of planetary building blocks during Solar System formation
Two-part formation of the Solar System
Measurements of meteorites have shown that the inner and outer Solar System formed from two distinct reservoirs of material. Existing models have proposed that these were split by Jupiter forming first, which would open a gap in the protoplanetary disc. Lichtenberg et al. instead argue that the snow line, the boundary between regions containing water vapor and solid ice, migrated first outward and then inward, forming two separate populations of planetesimals. Those planetesimals then grew through collisions to form the planets. Their simulation of this model explains the meteorite data and is consistent with astronomical observations of protoplanetary disks around other stars.
Science, this issue p. 365
Abstract
Geochemical and astronomical evidence demonstrates that planet formation occurred in two spatially and temporally separated reservoirs. The origin of this dichotomy is unknown. We use numerical models to investigate how the evolution of the solar protoplanetary disk influenced the timing of protoplanet formation and their internal evolution. Migration of the water snow line can generate two distinct bursts of planetesimal formation that sample different source regions. These reservoirs evolve in divergent geophysical modes and develop distinct volatile contents, consistent with constraints from accretion chronology, thermochemistry, and the mass divergence of inner and outer Solar System. Our simulations suggest that the compositional fractionation and isotopic dichotomy of the Solar System was initiated by the interplay between disk dynamics, heterogeneous accretion, and internal evolution of forming protoplanets.
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Supplementary Material
Summary
Materials and Methods
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References and Notes
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Volume 371 | Issue 6527
22 January 2021
22 January 2021
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Copyright © 2021, American Association for the Advancement of Science.
This is an article distributed under the terms of the Science Journals Default License.
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Received: 2 March 2020
Accepted: 10 December 2020
Published in print: 22 January 2021
Acknowledgments
We thank C. P. Dullemond, A. C. Hunt, I. Pascucci, S. Ida, J. Wade, S.-J. Paardekooper, T. Birnstiel, S. M. Stammler, J. J. Barnes, A. Morbidelli, W. Kley, and members of the ERC EXOCONDENSE project at Oxford for discussions; B. Liu, J. F. J. Bryson, M. Ek, R. D. Alexander, and S. Charnoz for comments on earlier draft versions; T. V. Gerya for usage of the I2ELVIS code family; and C. P. Dullemond for usage of the disk evolution code. Funding: T.L. received funding from the Simons Foundation (SCOL award no. 611576) and the Swiss National Science Foundation (grant no. P2EZP2-178621). J.D. received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation program (grant no. 714769). T.O.H. was supported by the University of Zurich Forschungskredit Postdoc. Parts of this work were carried out within the framework of the National Centre for Competence in Research PlanetS (grant no. 51NF40-141881) supported by the Swiss National Science Foundation. Author contributions: Conceptualization, T.L., J.D., M.S., G.J.G.; Methodology, T.L., J.D., T.O.H., G.J.G.; Software, T.L., J.D., T.O.H., G.J.G.; Validation, all authors; Formal Analysis, T.L., J.D., T.O.H.; Investigation, T.L., J.D., M.S.; Resources, T.L., J.D., M.S.; Writing, T.L., J.D., T.O.H., M.S.; Review & Editing, all authors; Visualization, T.L. Competing interests: We declare no competing interests. Data and materials availability: The simulation codes, output data, and plotting scripts are available at https://osf.io/e2kfv.
Authors
Funding Information
Simons Foundation: 611576
H2020 European Research Council: 714769
Swiss National Science Foundation: P2EZP2-178621
Swiss National Science Foundation: 51NF40-141881
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