The formation of Uranus and Neptune in the Jupiter–Saturn region of the Solar System (original) (raw)

Nature volume 402, pages 635–638 (1999)Cite this article

Abstract

Planets are believed to have formed through the accumulation of a large number of small bodies1,2,3,4. In the case of the gas-giant planets Jupiter and Saturn, they accreted a significant amount of gas directly from the protosolar nebula after accumulating solid cores of about 5–15 Earth masses5,6. Such models, however, have been unable to produce the smaller ice giants7,8 Uranus and Neptune at their present locations, because in that region of the Solar System the small planetary bodies will have been more widely spaced, and less tightly bound gravitationally to the Sun. When applied to the current Jupiter–Saturn zone, a recent theory predicts that, in addition to the solid cores of Jupiter and Saturn, two or three other solid bodies of comparable mass are likely to have formed9. Here we report the results of model calculations that demonstrate that such cores will have been gravitationally scattered outwards as Jupiter, and perhaps Saturn, accreted nebular gas. The orbits of these cores then evolve into orbits that resemble those of Uranus and Neptune, as a result of gravitational interactions with the small bodies in the outer disk of the protosolar nebula.

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References

  1. Safronov,V. S. Evolution of the Protoplanetary Cloud and the Formation of the Earth and Planets (Nauka, Moscow, 1969).
    Google Scholar
  2. Wetherill,G. W. An alternative model for the formation of the asteroids. Icarus 100, 307–325 (1992).
    Article ADS Google Scholar
  3. Chambers,J. E. & Wetherill,G. W. Making the terrestrial planets: N-body integrations of planetary embryos in three dimensions. Icarus 136, 304–327 (1999).
    Article ADS Google Scholar
  4. Agnor,C. B., Canup,R. & Levison,H. On the character and consequences of large impacts in the late stage of terrestrial planet formation. Icarus 142, 219–237 (1999).
    Article ADS Google Scholar
  5. Bodenheimer,P. & Pollack,J. B. Calculations of the accretion and evolution of giant planets: the effects of solid cores. Icarus 67, 391–408 (1986).
    Article ADS Google Scholar
  6. Pollack,J. B. et al. Formation of the giant planets by concurrent accretion of solids and gas. Icarus 124, 62–85 (1996).
    Article ADS Google Scholar
  7. Lissauer,J. J., Pollack,J. B., Wetherill,G. W. & Stevenson,D. J. in Neptune and Triton (ed. Cruikshank, D. P.) 37–108 (Univ. Arizona Press, Tucson, 1996).
    Google Scholar
  8. Stewart,G. & Levison,H. F. On the formation of Uranus and Neptune. Proc. Lunar Planet. Sci. Conf. XXIX, abstr. no. 1960 (1998).
  9. Kokubo,E. & Ida,S. Oligarchic growth of protoplanets. Icarus 131, 171–178 (1998).
    Article ADS Google Scholar
  10. Morbidelli,A. in Solar System Formation and Evolution (eds. Lazzaro, D., Vieira Martins, R., Ferraz-Mello, S., Fernandez, J. & Beauge, C.) 83 (ASP Conf. Ser. 149, 1998).
    Google Scholar
  11. Levison,H. & Duncan,M. From the Kuiper belt to Jupiter-family comets: the spatial distribution of ecliptic comets. Icarus 127, 13–32 (1997).
    Article ADS Google Scholar
  12. Duncan,M. & Levison,H. F. A scattered disk of icy objects and the origin of Jupiter-family comets. Science 276, 1670–1672 (1997).
    Article ADS CAS Google Scholar
  13. Luu,J. et al. A new dynamical class of object in the outer Solar System. Nature 387, 573–575 (1997).
    Article ADS CAS Google Scholar
  14. Fernandez,J. A. & Ip,W.-H. Some dynamical aspects of the accretion of Uranus and Neptune—The exchange of orbital angular momentum with planetesimals. Icarus 58, 109–120 (1984).
    Article ADS Google Scholar
  15. Hahn,J. & Malhotra,R. Radial migration of planets embedded in a massive planetesimal disk. Astron. J. 117, 3041–3053 (1999).
    Article ADS Google Scholar
  16. Rasio,F. A. & Ford,E. B. Dynamical instabilities and the formation of extrasolar planetary systems. Science 274, 954–956 (1996).
    Article ADS CAS Google Scholar
  17. Weidenschilling,S. J. & Marzari,F. Gravitational scattering as a possible origin for giant planets at small stellar distances. Nature 384, 619–621 (1996).
    Article ADS CAS Google Scholar
  18. Lin,D. N. C. & Ida,S. On the origin of massive eccentric planets. Astrophys. J. 477, 781–791 (1997).
    Article ADS CAS Google Scholar
  19. Levison,H. F., Lissauer,J. J. & Duncan,M. J. Modeling the diversity of outer planetary systems. Astron. J. 116, 1998–2014 (1998).
    Article ADS Google Scholar
  20. Duncan,M., Levison,H. & Lee,M. H. A multiple timestep symplectic algorithm for integrating close encounters. Astron. J. 116, 2067–2077 (1998).
    Article ADS Google Scholar
  21. Malhotra,R. The origin of Pluto's orbit: implications for the Solar System beyond Neptune. Astron. J. 110, 420–429 (1995).
    Article ADS Google Scholar

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Acknowledgements

We thank G. Stewart and K. Zahnle for discussions, and L. Dones, B. Gladman, W. McKinnon, J. Parker, A. Stern, W. Ward and G. Wetherill for comments on an earlier draft. E.W.T. and M.J.D. were supported by the Natural Science and Engineering Research Council of Canada, H.F.L. was supported by NASA's Planetary Geology & Geophysics, Origins of Solar Systems, and Exobiology programme.

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Authors and Affiliations

  1. Department of Physics, Queen's University, Kingston, K7L 3N6, Ontario, Canada
    Edward W. Thommes & Martin J. Duncan
  2. Space Studies Department, Southwest Research Institute, Boulder, 80302, Colorado, USA
    Harold F. Levison

Authors

  1. Edward W. Thommes
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  2. Martin J. Duncan
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  3. Harold F. Levison
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Corresponding author

Correspondence toMartin J. Duncan.

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Thommes, E., Duncan, M. & Levison, H. The formation of Uranus and Neptune in the Jupiter–Saturn region of the Solar System.Nature 402, 635–638 (1999). https://doi.org/10.1038/45185

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