2011ApJ...729...98P

If the two planets in the HAT-P-13 system are coplanar, the orbital states provide a probe of the internal planetary structure. Previous analyses of radial velocity and transit timing data for the system suggested that the observational constraints on the orbital states were rather small. We reanalyze the available data, treating the jitter as an unknown MCMC parameter, and find that a wide range of jitter values are plausible, hence the system parameters are less well constrained than previously suggested. For slightly increased levels of jitter (∼4.5 m/s), the eccentricity of the inner planet can be in the range 0 < e_inner< 0.07, the period and eccentricity of the outer planet can be 440 days < P_outer< 470 days and 0.55 < e_outer < 0.85, respectively, while the relative pericenter alignment, η, of the planets can take essentially any value -180° < η < +180°. It is therefore difficult to determine whether e_inner and η have evolved to a fixed-point state or a limit cycle or to use e_inner to probe the internal planetary structure. We perform various transit timing variation (TTV) analyses, demonstrating that current constraints merely restrict e_outer< 0.85, and rule out relative planetary inclinations within ∼2° of i_rel= 90°, but that future observations could significantly tighten the restriction on both these parameters. We demonstrate that TTV profiles can readily distinguish the theoretically favored inclinations of i_rel= 0° and 45°, provided that sufficiently precise and frequent transit timing observations of HAT-P-13b can be made close to the pericenter passage of HAT-P-13c. We note the relatively high probability that HAT-P-13c transits and suggest observational dates and strategies.