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Exploring S-type orbits in the Pluto-Charon binary system
(Wiley-Blackwell, 2010-05-01)
This work generates, through a sample of numerical simulations of the restricted three-body problem, diagrams of semimajor axis and eccentricity which defines stable and unstable zones for particles in S-type orbits around ...
Exploring S-type orbits in the Pluto-Charon binary system
(Wiley-Blackwell, 2010-05-01)
This work generates, through a sample of numerical simulations of the restricted three-body problem, diagrams of semimajor axis and eccentricity which defines stable and unstable zones for particles in S-type orbits around ...
Semianalytical model for planetary resonances: Application to planets around single and binary stars
(EDP Sciences, 2021-02)
Context. Planetary resonances are a common dynamical mechanism acting on planetary systems. However, no general model for describing their properties exists, particularly for commensurabilities of any order and arbitrary ...
Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
(2019-07-01)
Super-Earths - planets with sizes between the Earth and Neptune - are found in tighter orbits than that of the Earth around more than one third of main sequence stars. It has been proposed that super-Earths are scaled-up ...
Formation of the Janus-Epimetheus system through collisions
(2015-11-01)
Context. Co-orbital systems are bodies that share the same mean orbit. They can be divided into different families according to the relative mass of the co-orbital partners and the particularities of their movement. Janus ...
Scattering V-type asteroids during the giant planet instability: a step for Jupiter, a leap for basalt
(Oxford Univ Press, 2017-06-01)
V-type asteroids are a taxonomic class whose surface is associated with a basaltic composition. The only known source of V-type asteroids in the Main Asteroid Belt is (4) Vesta, which is located in the inner part of the ...
Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains
(2021-06-01)
At least 30% of main sequence stars host planets with sizes of between 1 and 4 Earth radii and orbital periods of less than 100 days.We use N-body simulations including a model for gas-assisted pebble accretion and disk–planet ...
An alternative stable solution for the Kepler-419 system, obtained with the use of a genetic algorithm
(EDP Sciences, 2018-11)
Context. The mid-Transit times of an exoplanet may be nonperiodic. The variations in the timing of the transits with respect to a single period, that is, the transit timing variations (TTVs), can sometimes be attributed ...