Small Body Populations in Systems with Two Eccentric Jupiter-Mass Planets.

ZANARDI, MACARENA; LI, GONGJIE; DE ELÍA, GONZALO CARLOS; NAOZ, SMADAR; DI SISTO, ROMINA P.

Montevideo

Congreso; Asteroid Comets Meteors 2017; 2017

Introduction: The number of confirmed planets discovered to date outside the Solar System ascends to 3313, of whom a high percentage are gas giants with masses greater than 1 MJup and with a wide range of eccentricities. One of the channels suggested in the literature that can explain the highly eccentric orbits of the observed exoplanets is known as planet-planet scattering [1,2]. These instability events produce crossing orbits and successive close encounters between planets, which could derive in the ejection of one or more of them as well as collisions with the central star. It is very interesting to analyze the final planetary architecture as well as the dynamical evolution of small body reservoirs in such scenarios of instability. A recent work [3] studied the dynamical effects of a single Jupitermass planet on an outer small body population after a planetary scattering event around stars of0.5 solar masses. According such a work, the surviving particles show different dynamical behaviours. In fact, those simulations produce particles on prograde and retrograde orbits, as well as particles whose orbital plane ?flips? from prograde to retrograde and back again alongtheir evolution. Such particles, which are called ?Type-F particles?, show strong correlations between their inclination and ascending node longitud. In the present research, we analyze the dynamical effects of two Jupiter-mass planets on small body populations in planetary scattering scenarios. Methods: To do this, we carry out N-body simulations assuming three Jupiter-mass planets close to their instability limit [4] together with an outer planetesimal disk. To model such a population, we use 1000 massless particles, which are distributed in a disk of 30 au from the central star. The present research analyses those numerical simulations in which two Jupitermass planets survive after the dynamical instability event. The N-body simulations are carriedout making use of the MERCURY code [5]. Results: The small body populations produced in the present study show a wide diversity ofdynamical behaviours. In particular, the surviving ?Type-F particles? show dynamical features very different in comparison with those derivedin systems with a single Jupiter-mass planet (see Fig. 1). A detailed dynamical analysis is developed in the present contribution.