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We provide evidence that the obliquities of stars with close-in giant planetswere initially nearly random, and that the low obliquities that are oftenobserved are a consequence of star-planet tidal interactions. The evidence isbased on 14 new measurements of the Rossiter-McLaughlin effect (for the systemsHAT-P-6, HAT-P-7, HAT-P-16, HAT-P-24, HAT-P-32, HAT-P-34, WASP-12, WASP-16,WASP-18, WASP-19, WASP-26, WASP-31, Gl 436, and Kepler-8), as well as acritical review of previous observations. The low-obliquity (well-aligned)systems are those for which the expected tidal timescale is short, and likewisethe high-obliquity (misaligned and retrograde) systems are those for which theexpected timescale is long. At face value, this finding indicates that theorigin of hot Jupiters involves dynamical interactions like planet-planetinteractions or the Kozai effect that tilt their orbits, rather thaninspiraling due to interaction with a protoplanetary disk. We discuss thestatus of this hypothesis and the observations that are needed for a moredefinitive conclusion.

Obliquities of Hot Jupiter host stars: Evidence for tidal interactions and primordial misalignments