The Architectures of Planetary Systems from Transit Observations

Details The Architectures of Planetary Systems from Transit Observations The Architectures of Planetary Systems from Transit Observations

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21710305f&link_type=abstract

American Astronomical Society, AAS Meeting #217, #103.05; Bulletin of the American Astronomical Society, Vol. 43, 2011

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The architectures of multiple planet systems can provide valuable constraints on models of planet formation, including the extent and cause of orbital migration, eccentricity excitation and inclination excitation. NASA's Kepler mission has discovered a planetary system with multiple transiting planets (Holman et al. 2010) and several stars with multiple transiting planet candidates (Steffen et al. 2010). For each planet, transit photometry can measure the orbital period, orbital phase, transit duration, planet size (relative to the host star), and, in favorable cases, the orbital inclination. For systems with multiple transiting planets, one can begin to piece together the architecture of the planetary system, including key features such as the proximity to mean motion resonance, potential for significant secular interactions, and the likely relative inclinations. The set of potential architectures can often be further narrowed by incorporating the constraint of long-term orbital stability (for plausible mass-radius relations) and/or incorporating complimentary observations (e.g., radial velocities, Rossiter-McLaughlin effect, transit timing, out-of-transit light curve). We describe the methodology for characterizing the architecture transiting planet systems and present early results of such analyses for the Kepler-9 system, as well as candidate multiple planet systems previously identified by Kepler. Funding for Kepler is provided by NASA's Science Mission Directorate and for this research by the Kepler Participating Scientist Program.

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