Volume 579, July 2015
|Number of page(s)||15|
|Section||Planets and planetary systems|
|Published online||23 June 2015|
Theoretical models of planetary system formation
II. Post-formation evolution
Physikalisches Institut & Center for Space and Habitability,
e-mail: firstname.lastname@example.org; WBenz;email@example.com
2 Observatoire de Besançon, 41 avenue de l’Observatoire, 25000 Besançon, France
Received: 28 May 2014
Accepted: 5 December 2014
Aims. We extend the results of planetary formation synthesis by computing the long-term evolution of synthetic systems from the clearing of the gas disk into the dynamical evolution phase.
Methods. We use the symplectic integrator SyMBA to numerically integrate the orbits of planets for 100 Myr, using populations from previous studies as initial conditions.
Results. We show that within the populations studied, mass and semimajor axis distributions experience only minor changes from post-formation evolution. We also show that, depending upon their initial distribution, planetary eccentricities can statistically increase or decrease as a result of gravitational interactions. We find that planetary masses and orbital spacings provided by planet formation models do not result in eccentricity distributions comparable to observed exoplanet eccentricities, requiring other phenomena, such as stellar fly-bys, to account for observed eccentricities.
Key words: planets and satellites: dynamical evolution and stability / planets and satellites: formation
© ESO, 2015
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