  Radial velocity observations from three instruments reveal the presence of a
4 M_jup planet candidate orbiting the K giant HD 76920. HD 76920b has an
orbital eccentricity of 0.856$\pm$0.009, making it the most eccentric planet
known to orbit an evolved star. There is no indication that HD 76920 has an
unseen binary companion, suggesting a scattering event rather than Kozai
oscillations as a probable culprit for the observed eccentricity. The candidate
planet currently approaches to about four stellar radii from its host star, and
is predicted to be engulfed on a $\sim$100 Myr timescale due to the combined
effects of stellar evolution and tidal interactions.
