The 3-Dimensional Architecture of the Upsilon Andromedae Planetary System
Draft version August 14, 2018 Preprint typeset using LATEX style emulateapj v. 04/17/13 THE 3-DIMENSIONAL ARCHITECTURE OF THE υ ANDROMEDAE PLANETARY SYSTEM Russell Deitrick Department of Astronomy, University of Washington, Seattle, WA 98195-1580, USA Rory Barnes Department of Astronomy, University of Washington, Seattle, WA 98195-1580, USA Barbara McArthur Department of Astronomy, University of Texas at Austin, TX 78712, USA Thomas R. Quinn Department of Astronomy, University of Washington, Seattle, WA 98195-1580, USA Rodrigo Luger Department of Astronomy, University of Washington, Seattle, WA 98195-1580, USA Adrienne Antonsen Department of Astronomy, University of Washington, Seattle, WA 98195-1580, USA and G. Fritz Benedict Department of Astronomy, University of Texas at Austin, TX 78712, USA (Dated:) Draft version August 14, 2018 ABSTRACT The Upsilon Andromedae system is the first exoplanetary system to have the relative inclination of two planets' orbital planes directly measured, and therefore offers our first window into the 3- dimensional configurations of planetary systems. We present, for the first time, full 3-dimensional, dynamically stable configurations for the 3 planets of the system consistent with all observational constraints. While the outer 2 planets, c and d, are inclined by ∼ 30◦, the inner planet's orbital plane has not been detected. We use N-body simulations to search for stable 3-planet configurations that are consistent with the combined radial velocity and astrometric solution. We find that only 10 trials out of 1000 are robustly stable on 100 Myr timescales, or ∼ 8 billion orbits of planet b. Planet b's orbit must lie near the invariable plane of planets c and d, but can be either prograde or retrograde.
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