Published in The Astrophysical Journal
We study the evolution of planetesimals in evolved gaseous disks that orbit a solar- mass star and harbor a Jupiter-mass planet at $a _ p\ approx 5$ AU. The gas dynamics are modeled with a three-dimensional hydrodynamics code that employs nested grids and achieves a resolution of one Jupiter radius in the circumplanetary disk. The code models solid...
Published in Icarus
We present calculations of the early stages of the formation of Jupiter via core nucleated accretion and gas capture. The core begins as a seed body of about 350 km in radius and orbits in a swarm of planetesimals whose initial radii range from 15 m to 50 km. The evolution of the swarm accounts for growth and fragmentation, viscous and gravitationa...
Numerical simulations show that a Jupiter mass planet is able to dig the gas material along its path. Resulting from this, a density gap is produced within the disk which may represent a large-scale density feature. Based on these hydrodynamical simulations we investigate the possibility to trace planets in circumstellar disks by means of infrared ...
Published in The Astrophysical Journal
Using detailed numerical simulations, we study the formation of bodies near the deuterium-burning limit according to the core-nucleated giant planet accretion scenario. The objects, with heavy-element cores in the range 5-30 M⊕, are assumed to accrete gas up to final masses of 10-15 Jupiter masses (M Jup). After the formation process, which lasts 1...
Published in The Astrophysical Journal
The outward migration of a pair of resonant-orbit planets, driven by tidal interactions with a gas-dominated disk, is studied in the context of evolved solar nebula models. The planets masses, M 1 and M 2, correspond to those of Jupiter and Saturn. Hydrodynamical calculations in two and three dimensions are used to quantify the migration rates and...
Published in The Astrophysical Journal
The increase of computational resources has recently allowed high-resolution, three-dimensional calculations of planets embedded in gaseous protoplanetary disks. They provide estimates of the planet migration timescale that can be compared to analytical predictions. While these predictions can result in extremely short migration timescales for core...
Published in The Astrophysical Journal
We analyze the gas accretion flow through a planet-produced gap in a protoplanetary disk. We adopt the α-disk model and ignore effects of planetary migration. We develop a semianalytic, one-dimensional model that accounts for the effects of the planet as a mass sink and also carry out two-dimensional hydrodynamic simulations of a planet embedded in...
Published in The Astrophysical Journal
Published in The Astrophysical Journal
With a series of numerical simulations, we analyze the thermohydrodynamic evolution of circumstellar disks containing Jupiter-sized protoplanets. In the framework of a two-dimensional approximation, we consider an energy equation that includes viscous heating and radiative effects in a simplified yet consistent form. Multiple nested grids are used ...
Published in The Astrophysical Journal
We investigate the evolution of protoplanets with different masses embedded in an accretion disk, via global fully three-dimensional hydrodynamical simulations. We consider a range of planetary masses extending from 1.5 M⊕ up to 1 MJ, and we take into account physically realistic gravitational potentials of forming planets. In order to calculate ac...
Published in arXiv preprint astro-ph/0208580
Planet evolution is tightly connected to the dynamics of both distant and close disk material. Hence, an appropriate description of disk-planet interaction requires global and high resolution computations, which we accomplish by applying a Nested-Grid method. Through simulations in two and three dimensions, we investigate how migration and accretio...
Published in ScienceOpen Astronomy & Astrophysics
We study the evolution of embedded protoplanets in a protostellar disk using very high resolution nested-grid computations. This method allows us to perform global simulations of planets orbiting in disks and, at the same time, to resolve in detail the dynamics of the flow inside the Roche lobe of the planet. The primary interest of this work lies ...
On the migration of protogiant solid cores FS Masset1,2 AIM - UMR 7158, CEA/CNRS/Univ. Paris 7, SAp, Orme des Merisiers, CE-Saclay, 91191 Gif/Yvette Cedex, France [email protected] G. D Angelo3 NASA-ARC, Space Science and Astrobiology Division, MS 245-3, Moffett Field, CA 94035, USA [email protected] and W. Kley Universit¨t T¨bingen, Institut f¨r ...
The aim of this dissertation is to study the dynamical interactions occurring between a forming planet and its surrounding protostellar environment. This task is accomplished by means of both two-and three-dimensional numerical simulations. In order to render the proper development of the work, results from such calculations are presented according...
Published in Exoplanets
Gas giant planets play a fundamental role in shaping the orbital architecture of planetary systems and in affecting the delivery of volatile materials to terrestrial planets in the habitable zones. Current theories of gas giant planet formation rely on either of two mechanisms: the core accretion model and the disk instability model. In this chapte...
Published in AGU Fall Meeting Abstracts
We are performing calculations of the formation of Jupiter via core nucleated accretion and gas capture. The calculations model the growth of a solid core from an evolving disk of planetesimals and the growth of a contracting gaseous envelope. We present results of the early phases of formation. The evolution of the solids accounts for growth and f...
Published in AGU Fall Meeting Abstracts
Recent simulations of the late stages growth of Jupiter presented by Lissauer et al.(2009, Icarus 199, 338) are used to test the model of capture of Jupiter s irregular satellites within proto-Jupiter s distended and thermally-supported envelope. We find such capture highly unlikely, since the envelope shrinks too slowly for a large number of moons...
Published in AGU Fall Meeting Abstracts
It has been proposed that the outward orbital migration of Jupiter and Saturn, driven by a gas-dominated protosolar disk, may help explain why they did not move much closer to the Sun. It has also been suggested that some properties of the inner Solar System may be interpreted by invoking an inward migration of Jupiter and Saturn followed by outwar...
207M 98. .1 ZOOOASPC. Stellar Clusters and Associations ASP Conference Series, Vol. 198, 2000 R. Pallavicini, G. Micela, and S. Sclortino, eds. Proper motions of X-ray detected stars in PSPC ROSAT pointed fields of Chamaeleon Region F. Morale, G. Micela, S. Sciortino Osservatorlo Astronomico di Palermo “GS. Vaiana”, Piazza del Parlamento 1, Palermo,...
