Resonances of Multiple Exoplanets and Implications for Their Formation

Abstract

Among $\sim 160$ of the multiple exoplanetary systems confirmed, about $30\%$ of them have neighboring pairs with a period ratio $\le 2$. A significant fraction of these pairs are around mean motion resonance (MMR), more interestingly, peak around 2:1 and 3:2, with a clear absence of more closely packed MMRs with period ratios less than 4:3, regardless of planet masses. Here we report numerical simulations demonstrating that such MMR behavior places important constraints on the disk evolution stage out of which the observed planets formed. Multiple massive planets (with mass $\ge 0.8$ $M_{\mathrm{Jup}}$) tend to end up with a 2:1 MMR mostly independent of the disk masses but low-mass planets (with mass $\le 30$ $M_{\oplus }$) can have MMRs larger than 4:3 only when the disk mass is quite small, suggesting that the observed dynamical architecture of most low-mass-planet pairs was established late in the disk evolution stage, just before it was dispersed completely.

5 pages, 5 figures, accepted for publication in ApJ Letters

References in corpus (5)

• A comparative study of disc-planet interaction
• Accretion in the Rho-Oph pre-main sequence stars
• Post-Oligarchic Evolution of Protoplanetary Embryos and the Stability of Planetary Systems
• Type I Planet Migration in Nearly Laminar Disks
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• Migration and Growth of Protoplanetary Embryos II: Emergence of Proto-Gas-Giants Cores versus Super Earths' Progenitor
• Terrestrial Planets Formation under Migration: the Systems near 4:2:1 Mean Motion Resonance
• The scattering outcomes of Kepler circumbinary planets: planet mass ratio