Planetesimal Evolution In Circumbinary Disks

Details Planetesimal Evolution In Circumbinary Disks Planetesimal Evolution In Circumbinary Disks

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.3205m&link_type=abstract

American Astronomical Society, DPS meeting #39, #32.05; Bulletin of the American Astronomical Society, Vol. 39, p.474

Astronomy and Astrophysics

Astronomy

Scientific paper

We adopt a hybrid approach to investigate the dynamical behaviour of planetesimals in a circumbinary disk. We compute the evolution of the gaseous component of the disk with the hydrodynamical code FARGO (Masset, 2000) modified to compute the disk evolution under the perturbations of a binary stellar system. The derived local gas density and velocity are then used to compute the drag force on planetesimals embedded in the disk at different distances from the barycenter of the stars. The relative impact velocities between planetesimals are estimated and compared with the accretion/erosion limiting velocity to test for the possibility of accretion and planet formation. The orbital evolution of planetesimals computed with the hybrid code is also compared to that derived from a simplified N--body code based on the axisymmetric approximation. The advantage of this last code is the limited amount of CPU required to compute a large number of planetesimal orbits.

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