SECULAR EVOLUTION OF HD 12661: A SYSTEM CAUGHT AT AN UNLIKELY TIME

@article{Veras2008SECULAREO,
  title={SECULAR EVOLUTION OF HD 12661: A SYSTEM CAUGHT AT AN UNLIKELY TIME},
  author={Dimitri Veras and Eric B. Ford},
  journal={The Astrophysical Journal},
  year={2008},
  volume={690},
  pages={L1 - L4}
}
  • D. VerasE. Ford
  • Published 31 October 2008
  • Geology, Physics
  • The Astrophysical Journal
The eccentricity evolution of multiple planet systems can provide valuable constraints on planet formation models. Unfortunately, the inevitable uncertainties in the current orbital elements can lead to significant ambiguities in the nature of the secular evolution. Integrating any single set of orbital elements inadequately describes the full range of secular evolutions consistent with current observations. Thus, we combine radial velocity observations of HD 12661 with Markov Chain Monte Carlo… 

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References

SHOWING 1-10 OF 27 REFERENCES

Planet–planet scattering in the upsilon Andromedae system

It is reported that the current orbital configuration of the three giant planets around upsilon Andromedae (υ And) probably results from a close dynamical interaction with another planet, now lost from the system, and shown that υ And c periodically returns to a very nearly circular state every 6,700 years.

Stability and formation of the resonant system HD 73526

Context. Based on radial velocity measurements, it has been found that the two giant planets detected around the star HD 73526 are in 2:1 resonance. However, as our numerical integration shows, the

Stability of the HD 12661 Planetary System

In this paper we study the stability of the HD 12661 planetary system in the framework of the N- body problem. Using the initial conditions found and announced by the California & Carnegie Planet

Extrasolar Planetary Dynamics with a Generalized Planar Laplace-Lagrange Secular Theory

The dynamical evolution of nearly half of the known extrasolar planets in multiple-planet systems may be dominated by secular perturbations. The commonly high eccentricities of the planetary orbits

Gravitational scattering as a possible origin for giant planets at small stellar distances

An alternative model for planetary migration that can account for two large orbital eccentricities of giant planets that are difficult to reconcile with a tidal-linkage model is described.

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

QUANTIFYING THE UNCERTAINTY IN THE ORBITS OF EXTRASOLAR PLANETS

Precise radial velocity measurements have led to the discovery of ∼100 extrasolar planetary systems. We investigate the uncertainty in the orbital solutions that have been fitted to these

Apsidal Alignment in υ Andromedae

One of the parameters fitted by Doppler radial velocity measurements of extrasolar planetary systems is ω, the argument of pericenter of a given planet's orbit referenced to the plane of the sky.

The Dynamics of the HD 12661 Extrasolar Planetary System

The main goal of this work is to analyze the possible dynamical mechanisms that dominate the motion of the HD 12661 extrasolar planetary system. By an analytical approach using the expansion of the

A dynamical mechanism for establishing apsidal resonance

We show that in a system of two planets initially in nearly circular orbits, an impulse perturbation that imparts a finite eccentricity to one planet's orbit causes the other planet's orbit to become