Volume 553, May 2013
|Number of page(s)||9|
|Section||Planets and planetary systems|
|Published online||06 May 2013|
Influence of the circumbinary disk gravity on planetesimal accumulation in the Kepler–16 system
1 Dipartimento di Fisica, University of Padova, via Marzolo 8, 35131 Padova, Italy
2 Observatoire de Paris, Section de Meudon, 92195 Meudon Principal Cedex, France
3 Observatoire de la Côte d’Azur, BP 4229, 06304 Nice Cedex, France
4 DAMTP, University of Cambridge, Wilberforce Road, Cambridge CB30 WA, UK
Received: 12 December 2012
Accepted: 18 March 2013
Context. Recent observations from NASA’s Kepler mission detected the first planets in circumbinary orbits. The question we try to answer is where these planets formed in the circumbinary disk and how far inside they migrated to reach their present location.
Aims. We investigate the first and most delicate phase of planet formation when planetesimals accumulate to form planetary embryos.
Methods. We use the hydrodynamical code FARGO to study the evolution of the disk and of a test population of planetesimals embedded in it. With this hybrid hydrodynamical-N-body code we can properly account for the gas drag force on the planetesimals and for the gravitational force of the disk on them.
Results. The numerical simulations show that the gravity of the eccentric disk on the planetesimal swarm excites their eccentricities to much higher values than those induced by the binary perturbations only within 10 AU from the stars. Moreover, the disk gravity prevents a full alignment of the planetesimal pericenters. Both these effects lead to high impact velocities, beyond the critical value for erosion.
Conclusions. Planetesimal accumulation in circumbinary disks appears to be prevented close to the stellar pair by the gravitational perturbations of the circumbinary disk. The observed planets possibly formed in the outer regions of the disk and then migrated inside by tidal interaction with the disk.
Key words: planet-disk interactions / planets and satellites: formation
© ESO, 2013
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