Application of Transit Timing Variations to the Detection of Exoplanets and the Determination of their Orbital and Structural Properties

Details Application of Transit Timing Variations to the Detection of Exoplanets and the Determination of their Orbital and Structural Properties Application of Transit Timing Variations to the Detection of Exoplanets and the Determination of their Orbital and Structural Properties

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dda....41.0404p&link_type=abstract

American Astronomical Society, DDA meeting #41, #4.04; Bulletin of the American Astronomical Society, Vol. 41, p.928

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Scientific paper

We expand upon the results of Veras at el. (2010) and investigate the practical utility of exo-planet transit timing variations (TTVs) in a number of different scenarios:
(i) We introduce significant non-coplanarity into our TTV investigations. This is because an increasing number of (Rossiter-McLaughlin) observations of transiting planets suggest that at least 10% of transiting planets are in retrograde orbits. We demonstrate that planets in retrograde orbits can frequently have significantly reduced TTVs, allowing the possibility that relatively massive, closely spaced systems of planets could escape detection via the TTV method
(ii) We apply the TTV method to the expected flood of Kepler detections, and ask whether the planets that are directly detected first by Kepler (hot-Jupiters and hot-Neptunes ) can be employed to indirectly detect Earth-mass planets in the habitable zone via the TTVs they induce in the inner planet. We show that this is indeed the case for certain systems, illustrating the dependencies on mass, inclination, eccentricity, etc , but place particular emphasis on the importance of long data streams
(iii) Finally, we turn to the specific example of the HAT-P-13 system, the first system in which a transiting planet is known to be accompanied by another planet in a well constrained orbit. We illustrate how observing TTVs in the inner planet can potentially constrain not only the eccentricity and the relative inclination of the (probably non-transiting) outer planet to the orbit of the inner planet , but potentially also the internal structure of the inner planet.

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