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• W194361685 abstract "We have simulated the last stage of planetary formation in the Cen binary system. We derive the possible sizes of terrestrial planets that can grow in spite of the gravitational perturbations of the companion star, and the amount of mass of the proto–planetary disk that falls onto the stars. In our simulations we also found a planetary system made of two planets locked in a 2:1 mean motion resonance, confirming that resonant configurations are common in planetary systems. At present the possible existence of planets around the stars of close binary systems is still matter of debate. Major questions on this topic are: can the gravitational perturbations from the companion star inhibit the accretion of planets? If not, what is the maximum size a planet can reach? During the formation process, do some planetary embryos fall into the stars increasing their metallicity? We have concentrated on the Alpha Centauri system, the prototype of close binary system with the more massive star very similar to our sun. According to [1], planetesimal accumulation in this system is possible around the primary star thanks to the coupling of two perturbing forces: gas drag and secular perturbations of the companion star. Planetary embryos are likely to form within 2 AU from the star in spite of the strong gravitational disturbance of the companion that, at perihelion, is only 11 AU far from the primary. To compute the outcome of the final stage of planetary formation when large embryos perturb each other in mutually crossing orbits and collide to form planets, we have numerically simulated the evolution of a 3–dimensional disk populated by 100–200 nearly coplanar planetary embryos. The secondary star, Cen B, is set at 23.4 AU from the primary on an eccentric orbit (e=0.52), all the protoplanets lay in the orbital plane of the binary system and move around the more massive star, Cen A. The orbits have been integrated with the Mercury package [2] for about 10 years. Collisions between embryos are assumed to be completely inelastic. To compute the initial distribution of embryos around the primary star, we have adopted a surface density of solid material equal to 8 g cm 2 at 1 AU, and decreasing as r . In the simulations we used different initial values for the embryo’s mass ranging from 0.75 ML ( 0:01M ) to 5.00 ML ( 0:06M ). The total mass in the embryos was about 75% of that expected in a disk with the above mentioned value of and ranged from 1.53 to 2.44 M , depending on the initial borders of the disk of planetary embryos. The maximum outer edge considered for the disk was 2.79 AU in agreement with the limit for orbital stability of [3], while the inner border was set to 0.4 AU. We assume that not all the mass of the disk is in protoplanets: a sensible fraction possibly remains in small planetesimals. The protoplanets radii are calculated assuming a density of 3 g cm . The initial eccentricities, e, are randomly selected in the range 0 e 0:04, the inclinations i in the range 0 i 0:01 . The remaining orbital elements are chosen randomly between 0 and 360. We assume that the planetary embryos formed via runaway growth and became dynamically isolated prior the start of our simulation. The initial separation between the planetary embryos, , is measured in mutual Hill radii: we varied the value of from 3 to 9." @default.
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• W194361685 date "2002-03-01" @default.
• W194361685 modified "2023-10-16" @default.
• W194361685 title "Planetary Formation, Resonances, and Star Mass Accretion in the Alpha Centauri System" @default.
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