Calculation of the enrichment of the giant planet envelopes during the "late heavy bombardment"

Abstract

The giant planets of our solar system possess envelopes consisting mainly of hydrogen and helium but are also significantly enriched in heavier elements relatively to our Sun. In order to better constrain how these heavy elements have been delivered, we quantify the amount accreted during the so-called "late heavy bombardment", at a time when planets were fully formed and planetesimals could not sink deep into the planets. On the basis of the "Nice model", we obtain accreted masses (in terrestrial units) equal to $0.15\pm 0.04{\mathrm{M}}_{\oplus }$ for Jupiter, and $0.08\pm 0.01{\mathrm{M}}_{\oplus }$ for Saturn. For the two other giant planets, the results are found to depend mostly on whether they switched position during the instability phase. For Uranus, the accreted mass is $0.051\pm 0.003{\mathrm{M}}_{\oplus }$ with an inversion and $0.030\pm 0.001{\mathrm{M}}_{\oplus }$ without an inversion. Neptune accretes $0.048\pm 0.015{\mathrm{M}}_{\oplus }$ in models in which it is initially closer to the Sun than Uranus, and $0.066\pm 0.006{\mathrm{M}}_{\oplus }$ otherwise. With well-mixed envelopes, this corresponds to an increase in the enrichment over the solar value of $0.033\pm 0.001$ and $0.074\pm 0.007$ for Jupiter and Saturn, respectively. For the two other planets, we find the enrichments to be $2.1\pm 1.4$ (w/ inversion) or $1.2\pm 0.7$ (w/o inversion) for Uranus, and $2.0\pm 1.2$ (w/ inversion) or $2.7\pm 1.6$ (w/o inversion) for Neptune. This is clearly insufficient to explain the inferred enrichments of $\sim 4$ for Jupiter, $\sim 7$ for Saturn and $\sim 45$ for Uranus and Neptune.

6 pages

References in corpus (6)

• Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune
• Accretion and destruction of planetesimals in turbulent disks
• Growth and migration of solids in evolving protostellar disks I: Methods and Analytical tests
• Dust accretion onto high-mass planets
• Coupling dynamical and collisional evolution of small bodies II : Forming the Kuiper Belt, the Scattered Disk and the Oort Cloud
• The Dynamical Structure of the Kuiper Belt and its Primordial Origin

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