This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.
Eric Ford (Penn State)
Abstract
Observations of strongly interacting planetary systems in or near a mean motion resonance are unusually sensitive to planet masses and orbital properties, including dynamical properties that can help illuminate planet formation. Having developed a powerful toolbox for translating Doppler and/or transit timing observations into physics parameters, now we are able to characterize the resonant and secular behaviour of several strongly interacting planetary systems. I will present recent results for selected resonant and near-resonant planetary systems and discuss implications for planet formation. In particular, I will address implications for the nature and extent of orbital migration for giant and low-mass planets.
Notes
- How didSTIPs form?
- Three strawman models:
- In situ formation: wrong
- Large-scale disk formation: wrong
- Nearly in situ formation plus modest early radial drift
- Three strawman models:
- STIP examples:
- GJ 876: 4 planets
- 55 Cnc: 5 planets, MMR
- … Meh.