Astronomy and Astrophysics – Astrophysics – Earth and Planetary Astrophysics
Scientific paper
2011-09-21
Astronomy and Astrophysics
Astrophysics
Earth and Planetary Astrophysics
Submitted to Astrophysical Journal
Scientific paper
Numerical simulations of the stochastic end stage of planet formation typically begin with a population of planetary embryos and planetesimals that grow into planets by merging. We analyzed the impact parameters of collisions leading to the growth of terrestrial planets from recent $N$-body simulations that assumed perfect merging and predicted the actual outcomes using a new analytic collision physics model. We find that collision outcomes are diverse and span all possible regimes: hit-and-run, merging, partial accretion, partial erosion, and catastrophic disruption. The primary outcomes of giant impacts between planetary embryos are approximately evenly split between partial accretion, graze-and-merge, and hit-and-run events. To explore the cumulative effects of more realistic collision outcomes, we modeled the growth of an individual terrestrial planet with a Monte Carlo technique using the distribution of impact parameters from $N$-body simulations. We find that fewer planets reached masses greater than $0.7 M_{\rm Earth}$ using the collision physics model compared to simulations that assumed every collision results in perfect merging. For final planets with masses of $0.7-1.5 M_{\rm Earth}$, 60% were enriched in their core-to-mantle mass fraction by $>10$% compared to the initial embryo composition. Fragmentation was significant ($\sim20$% of the final mass) and occurred primarily by erosion of the smaller body in partial accretion and hit-and-run events. In partial accretion events, the target body grows by preferentially accreting the iron core of the projectile and the escaping fragments are derived primarily from the silicate mantles of both bodies. Thus, the bulk composition of a planet can evolve via stochastic giant impacts.
Leinhardt Zoë M.
Stewart Sarah T.
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