| People | Locations | Statistics |
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| Naji, M. |
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| Motta, Antonella |
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| Aletan, Dirar |
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| Mohamed, Tarek |
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| Ertürk, Emre |
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| Taccardi, Nicola |
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| Kononenko, Denys |
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| Petrov, R. H. | Madrid |
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| Alshaaer, Mazen | Brussels |
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| Bih, L. |
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| Casati, R. |
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| Muller, Hermance |
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| Kočí, Jan | Prague |
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| Šuljagić, Marija |
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| Kalteremidou, Kalliopi-Artemi | Brussels |
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| Azam, Siraj |
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| Ospanova, Alyiya |
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| Blanpain, Bart |
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| Ali, M. A. |
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| Popa, V. |
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| Rančić, M. |
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| Ollier, Nadège |
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| Azevedo, Nuno Monteiro |
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| Landes, Michael |
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| Rignanese, Gian-Marco |
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Marzari, F.
in Cooperation with on an Cooperation-Score of 37%
Topics
Publications (4/4 displayed)
- 2021Influence of the body composition on the evolution of ejecta in the Didymos-Dimorphos binary system
- 2021Influence of the body composition on the evolution of ejecta in the Didymos-Dimorphos binary system
- 2010A peculiar family of Jupiter Trojans: The Eurybatescitations
- 2004Planetary formation and orbital stability in the gamma Cephei system
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article
Planetary formation and orbital stability in the gamma Cephei system
Abstract
We numerically investigated under which conditions the giant planet detected in the gammaCephei system could form in the core accretion scenario despite the presence of the very close companion star. In our study we modeled the accretion of large planetary embryos by using of a N-body symplectic mapping code adapted to S type binary star system. We also studied the dynamical stability of the giant planet orbit by using the FMA method of Laskar, testing its reliability in such a scenario. Our results show that, under the assumption of a massive protoplanetary disk, the core accretion model can explain the formation of the planet. The final semimajor axis results quite sensitive to the initial density profile assumed for the dust component of the disk.