Diversity and Origin of 2 : 1 Orbital Resonances in Extrasolar Planetary Systems

• DOI: 10.1086/422166
• Publication Date: 2004-08-10T14:01:01Z
• Authors: Man Hoi Lee
• Keywords: Celestial Mechanics; Astrophysics (astro-ph); 0103 physical sciences; Planetary Systems; FOS: Physical sciences; Planets And Satellites: General; Astrophysics; 01 natural sciences; 531

(Abridged) A diversity of 2:1 resonance configurations can be expected in extrasolar planetary systems, and their geometry can provide information about the origin of the resonances. Assembly during planet formation by the differential migration of planets due to planet-disk interaction is one scenario for the origin of mean-motion resonances in extrasolar planetary systems. The stable 2:1 resonance configurations that can be reached by differential migration of planets with constant masses and initially coplanar and nearly circular orbits are (1) anti-symmetric configurations with the mean-motion resonance variables theta_1 and theta_2 (in deg.) librating about 0 and 180, respectively (as in the Io-Europa pair), (2) symmetric configurations with both theta_1 and theta_2 librating about 0 (as in the GJ 876 system), and (3) asymmetric configurations with theta_1 and theta_2 librating about angles far from either 0 or 180. There are, however, stable 2:1 resonance configurations with symmetric (theta_1 = theta_2 = 0), asymmetric, and anti-symmetric (theta_1 = 180 and theta_2 = 0) librations that cannot be reached by differential migration of planets with constant masses and initially coplanar and nearly circular orbits. If real systems with these configurations are ever found, their origin would require (1) a change in the planetary mass ratio m_1/m_2 during migration, (2) a migration scenario involving inclination resonances, or (3) multiple-planet scattering in crowded planetary systems. We find that the asymmetric configurations with large e_2 and the theta_1 = 180 and theta_2 = 0 configurations have intersecting orbits and that the theta_1 = theta_2 = 0 configurations with e_1 > 0.714 have prograde periapse precessions.<br/>24 pages, including 14 figures; uses AASTeX v5.0; accepted for publication in ApJ<br/>