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We report the discovery of Kepler-432b, a giant planet ($M_b =5.41^{+0.32}_{-0.18} M_{\rm Jup}, R_b = 1.145^{+0.036}_{-0.039} R_{\rm Jup}$)transiting an evolved star $(M_\star = 1.32^{+0.10}_{-0.07} M_\odot, R_\star =4.06^{+0.12}_{-0.08} R_\odot)$ with an orbital period of $P_b =52.501129^{+0.000067}_{-0.000053}$ days. Radial velocities (RVs) reveal thatKepler-432b orbits its parent star with an eccentricity of $e =0.5134^{+0.0098}_{-0.0089}$, which we also measure independently withasterodensity profiling (AP; $e=0.507^{+0.039}_{-0.114}$), thereby confirmingthe validity of AP on this particular evolved star. The well-determinedplanetary properties and unusually large mass also make this planet animportant benchmark for theoretical models of super-Jupiter formation.Long-term RV monitoring detected the presence of a non-transiting outer planet(Kepler-432c; $M_c \sin{i_c} = 2.43^{+0.22}_{-0.24} M_{\rm Jup}, P_c =406.2^{+3.9}_{-2.5}$ days), and adaptive optics imaging revealed a nearby(0\farcs87), faint companion (Kepler-432B) that is a physically bound M dwarf.The host star exhibits high signal-to-noise asteroseismic oscillations, whichenable precise measurements of the stellar mass, radius and age. Analysis ofthe rotational splitting of the oscillation modes additionally reveals thestellar spin axis to be nearly edge-on, which suggests that the stellar spin islikely well-aligned with the orbit of the transiting planet. Despite its longperiod, the obliquity of the 52.5-day orbit may have been shaped by star-planetinteraction in a manner similar to hot Jupiter systems, and we presentobservational and theoretical evidence to support this scenario. Finally, as ashort-period outlier among giant planets orbiting giant stars, study ofKepler-432b may help explain the distribution of massive planets orbiting giantstars interior to 1 AU.

Kepler-432: a red giant interacting with one of its two long period giant planets