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Contributions > By speaker > Morgan Marvin

Constraining the Migration Channels of Warm Jupiters Using Population-Level Eccentricities
Marvin Morgan  1@  , Brendan P. Bowler  2  , Quang H. Tran  3  
1 : The University of Texas at Austin
2 : University of California, Santa Barbara
3 : Yale University

Giant planets are expected to predominantly form beyond the water ice line and occasionally undergo inward migration. Unlike hot Jupiters, which can result from high-eccentricity tidal migration, warm Jupiters between 0.1-1 AU are in many ways more challenging to explain because they reside outside the tidal influence of their host stars. Orbital eccentricities offer clues about the formation and evolution of warm Jupiters. Based on uniform Keplerian fits of 18,561 RVs targeting 200 warm Jupiters, we use hierarchical Bayesian modeling to evaluate the impact of host star metallicity, mass, and orbital separation on the reconstructed population-level eccentricity distributions. I will present results showing that ~25% of warm Jupiters have eccentricities consistent with near-circular orbits, suggesting that most warm Jupiters detected are dynamically hot. Warm Jupiters orbiting metal-rich stars are more eccentric than those orbiting metal-poor stars but no differences are observed as a function of stellar host mass or orbital separation. These results are broadly consistent with planet scattering shaping the orbits of close-in giants.

 
 

 

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