Astronomy and Astrophysics – Astronomy
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dda....39.1702l&link_type=abstract
American Astronomical Society, DDA meeting #39, #17.02
Astronomy and Astrophysics
Astronomy
Scientific paper
We present results from a series of direct N-body simulations of terrestrial planet formation. These simulations focus on determining the effect of the initial dust distribution on planetesimal growth in the middle phase of planet formation. The initial conditions include a range of initial dust mass from zero to ten times the initial planetesimal mass. All planetesimals are treated as gravitational aggregates. The planetesimal collision model allows both accretion and fragmentation outcomes. The dust interacts with the planetesimals through accretion and dynamical friction.
We find that when dynamical friction from the dust is included, the evolution of the planetesimals is slower and occurs more uniformly over semi-major axis. Because the dynamical friction causes the orbits of the planetesimals to circularize, the collisions between planetesimals are slow and always result in growth. As a result, the dust is not replenished. However, the dust is not accreted quickly and remains until late times. Eventually, the eccentricity of the largest objects can not be damped by the dust but instead begins to increase along with the impact speeds. In conclusion, we find that the middle phase of planet formation cannot produce a massive dust disk but if the debris is the result of an earlier phase it may have significant dynamical and evolutionary effects on the growth of planetesimals in the terrestrial region.
Leinhardt Zoe
Richardson Chris D.
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