On the Frequency of Additional Planets in Short Period Hot Jupiter Systems from Transit Timing Variations

Details On the Frequency of Additional Planets in Short Period Hot Jupiter Systems from Transit Timing Variations On the Frequency of Additional Planets in Short Period Hot Jupiter Systems from Transit Timing Variations

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21840605d&link_type=abstract

American Astronomical Society, AAS Meeting #218, #406.05; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

The large number of hot Jupiter planets allows one to probe these systems for additional unseen planets via transit timing variations (TTVs). Even relatively small terrestrial planets, when placed in an energetically favorable mean motion resonance (MMR), can cause detectable TTVs with an amplitude of several minutes (Holman and Murray 2005, Agol et al. 2005). In an effort to discover and characterize such companions, we have embarked on a systematic study of known transiting hot Jupiters, utilizing the 1.55 meter Kuiper telescope on Mt. Bigelow to measure multiple individual transits in an observing season to within 30 second precision, and constrain the nature of any planetary companions. Here, we present current and preliminary results on this study, and show that the systems HAT-P-5, HAT- P-6, HAT-P-8, HAT-P-9, WASP-11/HAT-P-10, HAT-P-11, TrES-2, and WASP-10 do not contain small mass companions in MMRs, or moderate mass companions in close enough proximity to induce TTVs on the order of 1.5 minutes.

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