Query : 2017A&A...607A..67M

2017A&A...607A..67M - Astronomy and Astrophysics, volume 607A, 67-67 (2017/11-1)

N-body simulations of planet formation via pebble accretion. I. First results.


Abstract (from CDS):

Context. Planet formation with pebbles has been proposed to solve a couple of long-standing issues in the classical formation model. Some sophisticated simulations have been performed to confirm the efficiency of pebble accretion. However, there has not been any global N-body simulations that compare the outcomes of planet formation via pebble accretion to observed extrasolar planetary systems.
Aims. In this paper, we study the effects of a range of initial parameters of planet formation via pebble accretion, and present the first results of our simulations.
Methods. We incorporate a published pebble-accretion model into the N-body code SyMBA, along with the effects of gas accretion, eccentricity and inclination damping, and planet migration in the disc.
Results. We confirm that pebble accretion leads to a variety of planetary systems, but have difficulty in reproducing observed properties of exoplanetary systems, such as planetary mass, semimajor axis, and eccentricity distributions. The main reason behind this is an overly efficient type-I migration, which closely depends on the disc model. However, our simulations also lead to a few interesting predictions. First, we find that formation efficiencies of planets depend on the stellar metallicities, not only for giant planets, but also for Earths (Es) and Super-Earths (SEs). The dependency for Es/SEs is subtle. Although higher metallicity environments lead to faster formation of a larger number of Es/SEs, they also tend to be lost later via dynamical instability. Second, our results indicate that a wide range of bulk densities observed for Es and SEs is a natural consequence of dynamical evolution of planetary systems. Third, the ejection trend of our simulations suggest that one free-floating E/SE may be expected for two smaller-mass planets.

Abstract Copyright: © ESO, 2017

Journal keyword(s): planets and satellites: formation - planets and satellites: dynamical evolution and stability - planetary systems - planets and satellites: general - protoplanetary disks - protoplanetary disks

Simbad objects: 3

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Number of rows : 3
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
1 BD+41 3306d Pl 19 19 00.5488384064 +41 38 04.581624991           ~ 31 0
2 BD+41 3306e Pl 19 19 00.5488384064 +41 38 04.581624991           ~ 36 0
3 BD+41 3306 PM* 19 19 00.5489000285 +41 38 04.582441681 10.01 9.67 8.86 8.18 7.66 K0V 269 0

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