Journal
ASTROPHYSICAL JOURNAL
Volume 750, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/750/2/106
Keywords
celestial mechanics; planets and satellites: detection; planets and satellites: dynamical evolution and stability; planets and satellites: formation; planet-star interactions
Categories
Funding
- NASA [NNX08AH83G]
- NASA through the Chandra X-ray Center [NAS8-03060]
- California Institute of Technology (Caltech)
- NASA [100340, NNX08AH83G] Funding Source: Federal RePORTER
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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) over dot alpha a(1/2) and consequently the number distribution satisfies dN/d log a alpha a(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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