Distinguishing Between Single Eccentric Planets And Planets In 2:1 Mean Motion Resonances

Details Distinguishing Between Single Eccentric Planets And Planets In 2:1 Mean Motion Resonances Distinguishing Between Single Eccentric Planets And Planets In 2:1 Mean Motion Resonances

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dda....40.0603m&link_type=abstract

American Astronomical Society, DDA meeting #40, #6.03; Bulletin of the American Astronomical Society, Vol. 41, p.899

Astronomy and Astrophysics

Astronomy

Scientific paper

The dynamical state of a multiple planet system can provide clues to its formation and orbital evolution. For example, slow, smooth, and convergent migration naturally leads to resonance capture, particularly for the 2:1 mean motion resonance. However, continued migration and/or planet-disk interactions could result in the system evolving out of resonance or becoming dynamically unstable. Thus, the prevalence of systems in various mean motion resonances and the libration amplitude about resonance will provide interesting constraints on planet formation models. Radial velocity surveys have discovered several systems that appear to be in or near a low-order mean motion resonance. We report on the development of a statistical framework to quantify the frequency of planets in or near mean motion resonances. This approach accounts for the possibility that some planetary systems currently believed to harbor a single eccentric planet might also contain a second planet with an orbital period near half that of the currently known planet. We report preliminary results for selected planetary systems.

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