Formation and Detectability of Terrestrial Planets around α Centauri B

@article{Guedes2008FormationAD,
  title={Formation and Detectability of Terrestrial Planets around $\alpha$ Centauri B},
  author={Javiera M. Guedes and Eugenio Jose Rivera and E. ScannapiecoM. Davis and Gregory P. Laughlin and Elisa V. Quintana and D. A. Fischer},
  journal={The Astrophysical Journal},
  year={2008},
  volume={679},
  pages={1582 - 1587}
}
We simulate the formation of planetary systems around α Centauri B. The N-body accretionary evolution of a Σ ∝ r−1 disk populated with 400-900 lunar-mass protoplanets is followed for 200 Myr. All simulations lead to the formation of multiple-planet systems with at least one planet in the 1-2 M⊕ mass range at 0.5-1.5 AU. We examine the detectability of our simulated planetary systems by generating synthetic radial velocity observations including noise based on the radial velocity residuals to… 

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References

SHOWING 1-10 OF 20 REFERENCES

Terrestrial Planet Formation in the α Centauri System

We examine the late stages of terrestrial planet formation around each star in the α Centauri A and α Centauri B binary system. Each integration begins with a "bimodal" mass distribution of 14 large

Terrestrial Planet Formation around Individual Stars within Binary Star Systems

We calculate herein the late stages of terrestrial planet accumulation around a solar-type star that has a binary companion with semimajor axis larger than the terrestrial planet region. We perform

An extrasolar planetary system with three Neptune-mass planets

Simulations show that the system of three Neptune-mass planets orbiting the nearby star HD 69830 is in a dynamically stable configuration and theoretical calculations favour a mainly rocky composition for both inner planets, while the outer planet probably has a significant gaseous envelope surrounding its rocky/icy core.

Making More Terrestrial Planets

The results of 16 new 3D N-body simulations of the final stage of the formation of the terrestrial planets are presented. These Nbody integrations begin with 150‐160 lunar-to-Mars size planetary

X-rays from α Centauri – The darkening of the solar twin

We present first results from five XMM-Newton observations of the binary system α Centauri, which has been observed in snapshot like exposures of roughly two hours each during the last two years. In

The planet search program at the ESO Coudé Echelle spectrometer - II. The $\alpha$ Centauri system: Limits for planetary companions

In this article we present the results of the planet search program carried out at the ESO Coudé Echelle Spectrometer (CES) for components A and B of the α Centauri system. Since November 1992 we

TERRESTRIAL PLANET FORMATION. I. THE TRANSITION FROM OLIGARCHIC GROWTH TO CHAOTIC GROWTH

We use a hybrid, multiannulus, n-body-coagulation code to investigate the growth of kilometer-sized planetesimals at 0.4-2 AU around a solar-type star. After a short runaway growth phase,

Habitable zones around main sequence stars.

The results suggest that mid-to-early K stars should be considered along with G stars as optimal candidates in the search for extraterrestrial life.

Are Proxima and α Centauri Gravitationally Bound

Using the most recent kinematic and radial velocity data in the literature, we calculate the binding energy of Proxima Centauri relative to the center of mass of the α Centauri system. When we adopt