Letter | Published:

Growing the gas-giant planets by the gradual accumulation of pebbles

Nature volume 524, pages 322324 (20 August 2015) | Download Citation

Abstract

It is widely held that the first step in forming gas-giant planets, such as Jupiter and Saturn, was the production of solid ‘cores’ each with a mass roughly ten times that of the Earth1,2. Getting the cores to form before the solar nebula dissipates (in about one to ten million years; ref. 3) has been a major challenge for planet formation models4,5. Recently models have emerged in which ‘pebbles’ (centimetre-to-metre-sized objects) are first concentrated by aerodynamic drag and then gravitationally collapse to form objects 100 to 1,000 kilometres in size6,7,8,9. These ‘planetesimals’ can then efficiently accrete left-over pebbles10 and directly form the cores of giant planets11,12. This model is known as ‘pebble accretion’; theoretically, it can produce cores of ten Earth masses in only a few thousand years11,13. Unfortunately, full simulations of this process13 show that, rather than creating a few such cores, it produces a population of hundreds of Earth-mass objects that are inconsistent with the structure of the Solar System. Here we report that this difficulty can be overcome if pebbles form slowly enough to allow the planetesimals to gravitationally interact with one another. In this situation, the largest planetesimals have time to scatter their smaller siblings out of the disk of pebbles, thereby stifling their growth. Our models show that, for a large and physically reasonable region of parameter space, this typically leads to the formation of one to four gas giants between 5 and 15 astronomical units from the Sun, in agreement with the observed structure of the Solar System.

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Acknowledgements

This work was supported by an NSF Astronomy and Astrophysics Research Grant (principal investigator H.F.L.). We thank A. Johansen, M. Lambrechts, A. Morbidelli, D. Nesvorny and C. Ormel for discussions.

Author information

Affiliations

  1. Southwest Research Institute and NASA Solar System Exploration Research Virtual Institute, 1050 Walnut Street, Suite 300, Boulder, Colorado 80302, USA

    • Harold F. Levison
    •  & Katherine A. Kretke
  2. Department of Physics, Engineering Physics, and Astronomy, Queen’s University, Kingston, Ontario K7L 3N6, Canada

    • Martin J. Duncan

Authors

  1. Search for Harold F. Levison in:

  2. Search for Katherine A. Kretke in:

  3. Search for Martin J. Duncan in:

Contributions

H.F.L. and K.A.K. jointly conceived of the paper and carried out the bulk of the numerical and semi-analytic calculations. M.J.D. developed a semi-analytic model of viscous stirring and growth rates in a population distribution. All authors contributed to the discussion of the results and to the crafting of the manuscript.

Competing interests

The authors declare no competing financial interests.

Corresponding author

Correspondence to Harold F. Levison.

Extended data

Supplementary information

Videos

  1. 1.

    The cumulative mass distribution of planetesimals and embryos

    The growth of planetary embryos in our fiducial simulation as illustrated by cumulative mass distributions. The initial distribution is shown in pale blue, while the evolving distribution is show in dark blue and red (for embryos larger than 1 Earth-masses). This is an animated version of Figure 1b in the main text.

  2. 2.

    The vertical distribution of pebbles and embryos.

    A comparison between the vertical distribution, as represented by tan(i), of pebbles (the time averaged cyan gradient) and embryos (black circles) as a function of time in the fiducial simulation. This is an animated version of Figure 2 in the main text.

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DOI

https://doi.org/10.1038/nature14675

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