Effects of an eccentric inner Jupiter on the dynamical evolution of icy body reservoirs in a planetary scattering scenario

ZANARDI, M.; DE ELÍA, G. C.; DI SISTO, R. P.; NAOZ, S.; LI, G.; GUILERA, O. M.; BRUNINI, A.

ASTRONOMY AND ASTROPHYSICS

EDP SCIENCES S A

Lugar: Paris; Año: 2017

0004-6361

Aims. We analyze the dynamics of small body reservoirs under the eects of an eccentric inner giant planet resulting from a planetaryscattering event around a 0.5 Msun star.Methods. First, we use a semi-analytical model to define the properties of the protoplanetary disk that lead to the formation of threeJupiter-mass planets. Then, we carry out N-body simulations assuming that the planets are close to their stability limit together with anouter planetesimal disk. In particular, the present work focuses on the analysis of N-body simulations in which a single Jupiter-massplanet survives after the dynamical instability event.Results. Our simulations produce outer small body reservoirs with particles on prograde and retrograde orbits, and other ones whoseorbital plane flips from prograde to retrograde and back again along their evolution (?Type-F particles?). We find strong correlationsbetween the inclination i and the ascending node longitude  of Type-F particles. First, librates around 90° or/and 270°. Thisproperty represents a necessary and sucient condition for the flipping of an orbit. Moreover, the libration periods of i and Omega areequal and they are out to phase by a quarter period. We also remark that the larger the libration amplitude of i, the larger the librationamplitude of Omega. We analyze the orbital parameters of Type-F particles immediately after the instability event (post IE parameters),when a single Jupiter-mass planet survives in the system. Our results suggest that the orbit of a particle can flip for any value of itspost IE eccentricity, although we find only two Type-F particles with post IE inclinations i <17°. Finally, our study indicates that theminimum value of the inclination of the Type-F particles in a given system decreases with an increase in the eccentricity of the giantplanet.