Journal
ASTROPHYSICAL JOURNAL
Volume 718, Issue 1, Pages 543-550Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/718/1/543
Keywords
methods: numerical; planets and satellites: detection
Categories
Funding
- NSF [AST-0449986]
- NASA Ames Astrobiology Institute [NNX08AY38A]
- NASA [NNX08AY38A, 92759] Funding Source: Federal RePORTER
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Transit timing variations (TTVs)-deviations from strict periodicity between successive passages of a transiting planet-can be used to probe the structure and dynamics of multiple-planet systems. In this paper, we examine prospects for numerically solving the so-called inverse problem, the determination of the orbital elements of a perturbing body from the TTVs it induces. We assume that the planetary systems under examination have a limited number of Doppler velocity measurements and show that a more extensive radial velocity (RV) characterization with precision comparable to the semi-amplitude of the perturber may remove degeneracies in the solution. We examine several configurations of interest, including (1) a prototypical non-resonant system, modeled after HD 40307 b and c, which contains multiple super-Earth-mass planets, (2) a hypothetical system containing a transiting giant planet with a terrestrial-mass companion trapped in low-order mean motion resonance, and (3) the HAT-P-13 system, in which forced precession by an outer perturbing body that is well characterized by Doppler RV measurements can give insight into the interior structure of a perturbing planet, and for which the determination of mutual inclination between the transiting planet and its perturber is a key issue.
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