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DOE OSTI · 22034523

SUPER-ECCENTRIC MIGRATING JUPITERS

Socrates, Aristotle·Katz, Boaz·Subo, Dong·Tremaine, Scott
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Abstract

An important class of formation theories for hot Jupiters involves the excitation of extreme orbital eccentricity (e = 0.99 or even larger) followed by tidal dissipation at periastron passage that eventually circularizes the planetary orbit at a period less than 10 days. In a steady state, this mechanism requires the existence of a significant population of super-eccentric (e > 0.9) migrating Jupiters with long orbital periods and periastron distances of only a few stellar radii. For these super-eccentric planets, the periastron is fixed due to conservation of orbital angular momentum and the energy dissipated per orbit is constant, implying that the rate of change in semi-major axis a is a-dot {proportional_to}a{sup 1/2} and consequently the number distribution satisfies dN/d log a{proportional_to}a{sup 1/2}. If this formation process produces most hot Jupiters, Kepler should detect several super-eccentric migrating progenitors of hot Jupiters, allowing for a test of high-eccentricity migration scenarios.

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79 ASTRONOMY AND ASTROPHYSICSASTRONOMYASTROPHYSICSDETECTIONDISTANCEDISTRIBUTIONEVOLUTIONEXCITATIONMECHANICSORBITAL ANGULAR MOMENTUMORBITSPLANETSSATELLITESSTABILITYSTARSSTEADY-STATE CONDITIONS

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Socrates, Aristotle, Katz, Boaz, Subo, Dong, Tremaine, Scott. 2012-05-10. SUPER-ECCENTRIC MIGRATING JUPITERS. https://doi.org/10.1088/0004-637x%2F750%2F2%2F106

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