Resonant Capture of Exoplanets Into the 3:2 Mean Motion Resonance

Details Resonant Capture of Exoplanets Into the 3:2 Mean Motion Resonance Resonant Capture of Exoplanets Into the 3:2 Mean Motion Resonance

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21734318r&link_type=abstract

American Astronomical Society, AAS Meeting #217, #343.18; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

Doppler observations have shown HD 45364 to harbor a multiple planet system with a 0.18 MJup planet interior to a 0.66 MJup planet. The orbital periods of these planets suggest that the system is in a 3:2 MMR (Correia et al. 2009). If we assume that these planets migrated through a gaseous protoplanetary disk into the 3:2 MMR observed today, then the current orbital properties can constrain the properties of the protoplanetary disk. We perform numerical experiments to explore the possible dynamical origins of the HD 45364 system. Using the FARGO hydrodynamic code (Masset 2000), we investigate to what degree disk parameters (e.g., viscosity and surface density profiles) dictate the final configuration of such systems.
Our numerical experiments frequently result in planetary systems participating in the 2:1 or 3:2 MMR's. For systems with a larger initial separation, MMRs are less frequent. We explore a range of disk parameters, but find none of these resulted in systems migrating through the 3:2 MMR. Higher disk viscosities led to longer-lived resonances. We present an example of disk parameters that results in a stable 3:2 MMR configuration (for integration time exceeding the viscous timescale of the disk) and is insensitive to initial position of the planets along their orbits.

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