A hot-Jupiter progenitor on a super-eccentric retrograde orbit.

ABSTRACT: Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations¹. These 'hot Jupiter' planets are instead thought to have migrated inward from beyond the ice line and several viable migration channels have been proposed, including eccentricity excitation through angular-momentum exchange with a third body followed by tidally driven orbital circularization^2,3. The discovery of the extremely eccentric (e = 0.93) giant exoplanet HD 80606 b (ref. ⁴) provided observational evidence that hot Jupiters may have formed through this high-eccentricity tidal-migration pathway⁵. However, no similar hot-Jupiter progenitors have been found and simulations predict that one factor affecting the efficacy of this mech

SUBMITTER: Gupta AF 

PROVIDER: S-EPMC11291287 | biostudies-literature | 2024 Jul

REPOSITORIES: biostudies-literature