Modeling Radial Velocity Data of Resonant Planets to Infer Migration Histories
arXiv:2005.03034 · doi:10.3847/1538-3881/aba751
Abstract
A number of giant planet pairs discovered by the radial velocity method with period ratios may reside in mean motion resonances. Convergent orbital migration and resonant capture at the time of formation would naturally explain the present-day resonant orbital configurations of these systems. Planets that experience smooth migration and eccentricity damping forces due to a proto-planetary disk should not only capture into mean motion resonances but also end up in a specific dynamical configuration within the resonance, sometimes referred to as apsidal corotation resonance (ACR). Here we develop a method for testing the hypothesis that a planet pair resides in an ACR by directly fitting radial velocity data. The ACR hypothesis strongly restricts the number of free parameters describing the radial velocity signal and we compare fits using this highly restricted model to fits using a more conventional two-planet RV model by using nested sampling simulations. We apply our method to HD 45364 and HD 33844, two systems hosting giant planet pairs in 3:2 and 5:3 resonances, respectively. We demonstrate that the observations of both systems support an ACR configuration and we use the results of our ACR model fits to constrain possible migration histories of these systems.
Revised in response to referee report and accepted to AJ; Code for RV fitting available online at https://github.com/shadden/ResonantPlanetPairsRVModeling
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- Detection of separatrices and chaotic seas based on orbit amplitudes
- Apsidal Alignment and Anti-Alignment of Planets in Mean-Motion Resonance: Disk-Driven Migration and Eccentricity Driving
- Periodic orbits in the 1:2:3 resonant chain and their impact on the orbital dynamics of the Kepler-51 planetary system
- exoMMR: a New Python Package to Confirm and Characterize Mean Motion Resonances
- Inferred Properties of Planets in Mean-Motion Resonances are Biased by Measurement Noise
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- The Effects of Disk Induced Apsidal Precession on Planets Captured into Mean Motion Resonance