Tides Alone Cannot Explain Kepler Planets Close to 2:1 MMR
Silburt et al
A number of Kepler planet pairs lie just wide of first-order mean motion resonances (MMRs). Tides have been frequently proposed to explain these pileups, but it is still an ongoing discussion. We contribute to this discussion by calculating an optimistic theoretical estimate on the minimum initial eccentricity required by Kepler planets to explain the current observed spacing, and compliment these calculations with N-body simulations. In particular, we investigate 27 Kepler systems having planets within 6% of the 2:1 MMR, and find that the initial eccentricities required to explain the observed spacings are unreasonable from simple dynamical arguments. Furthermore, our numerical simulations reveal resonant tugging, an effect which conspires against the migration of resonant planets away from the 2:1 MMR, requiring even higher initial eccentricities in order to explain the current Kepler distribution. Overall, we find that tides alone cannot explain planets close to 2:1 MMR, and additional mechanisms are required to explain these systems.
Tuesday, September 15, 2015
Tides Cannot Explain Kepler Exoplanets in 2:1 Orbital Resonances
Posted by Will Baird at 4:00 PM
Subscribe to: Post Comments (Atom)
Post a Comment
Note: Only a member of this blog may post a comment.