Research ArticleASTRONOMY

Timing of the formation and migration of giant planets as constrained by CB chondrites

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Science Advances  09 Dec 2016:
Vol. 2, no. 12, e1601658
DOI: 10.1126/sciadv.1601658
  • Fig. 1 Impact velocities on growing planetary embryos in the inner solar system.

    (A) Impact velocity from a canonical accretion simulation. (B to D) Impact velocities for models in which Jupiter begins a 100,000-year inward migration to 1.5 AU at 2, 4, and 6 My, respectively, before migrating out to its current position on a time scale of 500,000 years. The gray line marks an impact velocity of 18 km/s with the box encompassing the full range of the uncertainty for incipient vaporization of iron in planetesimal cores, including the effect of impact angle (18 ± 5 km/s). All impacts onto bodies larger than 1400 km in diameter are plotted.

  • Fig. 2 Impact velocities in a dynamically excited main asteroid belt disk.

    Impactor (A) and target (B) diameters are indicated by the color bar and marker size. The gray line marks an impact velocity of 18 km/s with the box encompassing the full range of the uncertainty for incipient vaporization of iron in planetesimal cores, including the effect of impact angle (18 ± 5 km/s). All impacts by bodies larger than 10 km in diameter are plotted.

Supplementary Materials

  • Supplementary material for this article is available at http://advances.sciencemag.org/cgi/content/full/2/12/e1601658/DC1

    Supplementary Materials and Methods

    fig. S1. Model setup for an excited post-migration main belt.

    fig. S2. Impact velocities in an excited post-migration main belt disk with no gas present.

    References (3638)

  • Supplementary Materials

    This PDF file includes:

    • Supplementary Materials and Methods
    • fig. S1. Model setup for an excited post-migration main belt.
    • fig. S2. Impact velocities in an excited post-migration main belt disk with no gas present.
    • References (36–38)

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