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Abstract: We simulate the formation of planetary systems around Alpha Centauri B. TheN-body accretionary evolution of a 1-r disk populated with 400-900 lunar-massprotoplanets is followed for 200 Myr. All simulations lead to the formation ofmultiple-planet systems with at least one planet in the 1-2 MEarth mass rangeat 0.5-1.5 AU. We examine the detectability of our simulated planetary systemsby generating synthetic radial velocity observations including noise based onthe radial velocity residuals to the recently published three planet fit to thenearby K0V star HD 69830. Using these synthetic observations, we find that wecan reliably detect a 1.8 MEarth planet in the habitable zone of Alpha CentauriB after only three years of high cadence observations. We also find that theplanet is detectable even if the radial velocity precision is 3 m-s, as long asthe noise spectrum is white. Our results show that the greatest uncertainty inour ability to detect rocky planets in the Alpha Centauri system is the unknownmagnitude of ultra-low frequency stellar noise.



Autor: Javiera M. Guedes, Eugenio J. Rivera, Erica Davis, Gregory Laughlin, Elisa V. Quintana, Debra A. Fischer

Fuente: https://arxiv.org/







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