Transit Timing Variations of Kepler Planets

Details Transit Timing Variations of Kepler Planets Transit Timing Variations of Kepler Planets

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21712103h&link_type=abstract

American Astronomical Society, AAS Meeting #217, #121.03; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Scientific paper

For a transiting planet following a fixed Keplerian ellipse, observers would measure a constant interval between successive transits. Orbital precession induced by general relativity, a planetary tidal bulge, or stellar oblateness could result in a variation of the transit interval for a planet with an eccentric or inclined orbit. Furthermore, tidal dissipation should alter the orbital period of the planet. These slow effects can only be detected over several years. However, the gravitational influence of other planets in the system can yield a detectable change in the transit interval over much shorter time scales. With the precision and continuous monitoring provided by Kepler photometry, the presence of sub-Earth mass planets in resonance, as well as larger planets at a wide range of orbital periods could, in principle, be readily detected. With the detection of transit timing variations in systems with multiple transiting bodies, such as Kepler-9, it is possible to establish from the transit observations alone that these bodies have planetary masses. But the combination of Kepler photometry with high-precision radial velocity observations is particularly powerful in establishing the orbital and physical properties of such systems. We will present the results of the analyses of transit timing variations in exoplanet systems observed by Kepler to date.
Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate.

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