Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.3307o&link_type=abstract
American Astronomical Society, ESS meeting #2, #33.07
Astronomy and Astrophysics
Astronomy
Scientific paper
We have investigated planetary accretion from planetesimals in the vicinity of central star through N-body simulations including gravitational interactions with disk gas. The increasing number of discovered extrasolar planets opens an opportunity for studies of new planet formation scenarios. Recent observations suggest that discovered super-Earths are generally not in resonant orbits and the averaged orbital radius is about 0.1 AU, well beyond the disk inner edge. Through a series of N-body simulations, we find that, in the case where the type I migration speed is reduced by a factor of 100 from that predicted by the linear theory, non-resonant solid planets are formed beyond 0.05 AU.
Using orbital integration and analytical arguments, we also find a new mechanism (an “eccentricity trap”) to halt type I migration of planets near the disk inner edge. In this mechanism, asymmetric eccentricity damping due to disk-planet interaction on the innermost planet at the disk edge plays a crucial role in the trap. This trap is so strong that the edge torque exerted on the innermost planet can completely halt type I migrations of many outer planets through mutual resonant perturbations. Consequently, the convoy stays outside the disk edge, as a whole. We derive semi-analytical formula for the condition for the eccentricity trap and predict how many planets are likely to be trapped. It can be responsible for the formation of non-resonant, multiple, close-in super-Earths.
Duncan Martin J.
Ida Shigeru
Ogihara Masahiro
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