Physics
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.6303k&link_type=abstract
American Astronomical Society, DPS meeting #38, #63.03; Bulletin of the American Astronomical Society, Vol. 38, p.610
Physics
Scientific paper
Our goal is to constrain the conditions under which planetesimals are able to accrete into terrestrial-type planets in systems containing giant planets, brown dwarfs, and/or companion stars. We have modified the PSI multi-zone accretion code (Weidenschilling et al. 1997;Icarus 128,429) to accurately compute the planetesimal forced orbital elements due to perturbations from one or more massive companions. Evolution of the planetesimal proper orbital elements includes effects of collisions, fragmentation, nebular gas drag, and mutual planetesimal perturbations (stirring and dynamical friction). The proper orientation angles (pericenter and node) arising from these effects are assumed to be randomly distributed. However, the forced elements due to the companion perturbations are not random, but cause the orbits to be aligned in phase. The effects of nebular gas drag also influence the alignment of the forced orbital elements. This alignment is an essential component of the physics of accretion in these systems, because it allows even planetesimals with high values of forced eccentricity to have relative velocities that are considerably lower than if the orbits had random phasing. The new code accounts for this non-random phasing of the forced orientation angles when calculating the relative velocities and collision rates of planetesimals. Their lower relative velocities favor accretion of planetesimals as opposed to erosive cratering or disruption, and may allow terrestrial planets to grow in relatively compact systems with massive companions. [This material is based upon work supported by NASA under grants NNG04GP56G and NNG04GI14G.]
Kortenkamp Stephen J.
Marzari Francesco
Weidenschilling Stuart J.
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