Eccentricity evolution of giant planet orbits due to circumstellar disk torques

@article{Moorhead2007EccentricityEO,
  title={Eccentricity evolution of giant planet orbits due to circumstellar disk torques},
  author={Althea V. Moorhead and Fred C. Adams},
  journal={Icarus},
  year={2007},
  volume={193},
  pages={475-484}
}

Orbital evolution of eccentric planets in radiative discs

Context. With an average eccentricity of about 0.29, the eccentricity distribution of extrasolar planets is markedly different from the solar system. Among other scenarios considered, it has been

Dynamical Outcomes of Planet-Planet Scattering

Observations in the past decade have revealed extrasolar planets with a wide range of orbital semimajor axes and eccentricities. Based on the present understanding of planet formation via core

Extrasolar Planet Eccentricities from Scattering in the Presence of Residual Gas Disks

Gravitational scattering between massive planets has been invoked to explain the eccentricity distribution of extrasolar planets. For scattering to occur, the planets must either form in—or migrate

Origins of Eccentric Extrasolar Planets: Testing the Planet-Planet Scattering Model

In planetary systems with two or more giant planets, dynamical instabilities can lead to collisions or ejections through strong planet-planet scattering. Previous studies for initial conditions with

Terrestrial planet formation in low-eccentricity warm-Jupiter systems

Context. Extrasolar giant planets are found to orbit their host stars with a broad range of semi-major axes 0.02 ≤ a ≤ 6 AU. Current theories suggest that giant planets orbiting at distances between

Highly inclined and eccentric massive planets - I. Planet-disc interactions

In the Solar System, planets have a small inclination with respect to the equatorial plane of the Sun, but there is evidence that in extrasolar systems the inclination can be very high. This

EFFECTS OF DYNAMICAL EVOLUTION OF GIANT PLANETS ON SURVIVAL OF TERRESTRIAL PLANETS

The orbital distributions of currently observed extrasolar giant planets allow marginally stable orbits for hypothetical, terrestrial planets. In this paper, we propose that many of these systems may

PLANET–PLANET SCATTERING IN PLANETESIMAL DISKS. II. PREDICTIONS FOR OUTER EXTRASOLAR PLANETARY SYSTEMS

We develop an idealized dynamical model to predict the typical properties of outer extrasolar planetary systems, at radii comparable to the Jupiter-to-Neptune region of the solar system. The model is

Dynamically Unstable Planetary Systems Emerging Out of Gas Disks

The discovery of over 400 extrasolar planets allows us to statistically test our understanding of the formation and dynamics of planetary systems via numerical simulations. Traditional N-body

A limit on eccentricity growth from global 3D simulations of disc-planet interactions

We present high resolution 3-D simulations of the planet-disc interaction using smoothed particle hydrodynamics, to investigate the possibility of driving eccentricity growth by this mechanism. For

Evolution of Giant Planets in Eccentric Disks

We investigate the interaction between a giant planet and a viscous circumstellar disk by means of high-resolution, two-dimensional hydrodynamic simulations. We consider planetary masses that range

Eccentricity Evolution for Planets in Gaseous Disks

At least several percent of solar-type stars possess giant planets. Surprisingly, most move on orbits of substantial eccentricity. We investigate the hypothesis that interactions between a giant

ORBITAL EVOLUTION AND MIGRATION OF GIANT PLANETS: MODELING EXTRASOLAR PLANETS

Giant planets in circumstellar disks can migrate inward from their initial (formation) positions. Radial migration is caused by inward torques between the planet and the disk, by outward torques

Resonant Inclination Excitation of Migrating Giant Planets

The observed orbits of extrasolar planets suggest that many giant planets migrate a considerable distance toward their parent star as a result of interactions with the protoplanetary disk and that

Orbital eccentricity growth through disc-companion tidal interaction

We investigate the driving of orbital eccentricity of giant protoplanets and brown dwarfs through disc-companion tidal interactions by means of two dimensional numerical simulations. We consider disc

Planets Orbiting Other Suns

After a century fraught with false claims, evidence for planets around other stars finally appears robust. Infrared imaging and spectroscopy of disks around stars foreshadow detailed models of the

Dynamical Instabilities and the Formation of Extrasolar Planetary Systems

The existence of a dominant massive planet, Jupiter, in our solar system, although perhaps essential for long-term dynamical stability and the development of life, may not be typical of planetary

Migration and dynamical relaxation in crowded systems of giant planets

On the tidal interaction between protostellar disks and companions

Formation of protoplanets and binary stars in a protostellar disk modifies the structure of the disk. Through tidal interactions, energy and angular momentum are transferred between the disk and