Abstract

Warm Jupiters with orbital periods of ~ 10-365 days reside beyond the region of tidal influence from their host stars and, unlike hot Jupiters, are not expected to experience tidal circularization and realignment. Orbital eccentricities and stellar obliquities can offer important clues about the formation and dynamical history of warm Jupiters because in situ formation and disk migration should imprint near-circular orbits and mutually aligned systems whereas planet scattering should excite eccentricities and produce misaligned systems. To establish the relative importance of giant planet migration channels, I will present initial results from the largest self-consistent and most statistically rigorous analysis of warm Jupiter eccentricities to date. We find that metallicity plays a larger role in shaping the underlying eccentricity distribution of warm Jupiters than stellar mass or final orbital distance. Additionally, we find an excess of warm Jupiters with nearly circular orbits in multi-planet systems compared to single-planet systems. I also will share results from our warm Jupiter obliquity analysis. We find that cool stars harboring hot Jupiters spanning a/R* = 3-20 (~ 0.01-0.1 AU) and warm Jupiters spanning a/R* = 20-400 (~ 0.1-1.9 AU) are mostly consistent with spin-orbit alignment. However, the similarity of hot and warm Jupiter misalignment rates suggests that either misalignments are primordial and originate in misaligned disks, or the same underlying processes that create misaligned hot Jupiters also lead to misaligned warm Jupiters.