Transiting circumbinary planets Kepler-34 b and Kepler-35 b. Finally, we estimate the radial velocity semi-amplitudes of each planet for use in follow-up observations. We calculate the Hill radius of each planet to determine the area of influence of the planet in which any attached moon may reside, then calculate the estimated angular separation of the moon and planet for future imaging missions. We estimate the mass of each planet candidate using the mass–radius relationship developed by Chen & Kipping. However, if each giant planet holds more than one moon, then the occurrence rates of moons in the HZ would be comparable to that of terrestrial planets, and could potentially exceed them. We compare this with previously estimated occurrence rates of terrestrial planets in the HZ of G, K, and M stars and find that if each giant planet has one large terrestrial moon then these moons are less likely to exist in the HZ than terrestrial planets. ) in the OHZ, and find a frequency of (6.5 ± 1.9)% for G stars, (11.5 ± 3.1)% for K stars, and (6 ± 6)% for M stars.We calculate the occurrence rates of giant planets (R p = 3.0–25 R ⊠These giant planets are potential hosts to large terrestrial satellites (or exomoons) which would also exist in the HZ. The Kepler mission found hundreds of planet candidates within the Habitable Zones (HZ) of their host star, including over 70 candidates with radii larger than three Earth radii (R ⊠Seperuelo Duarte, Eduardo Kopparapu, Ravi K. Finally, as a short-period outlier among giant planets orbiting giant stars, study of Kepler-432b may help explain the distribution of massive planets orbiting giant stars interior to 1 AU.Įxploring Kepler Giant Planets in the Habitable Zone Despite its long period, the obliquity of the 52.5 day orbit may have been shaped by star- planet interaction in a manner similar to hot Jupiter systems, and we present observational and theoretical evidence to support this scenario. Analysis of the rotational splitting of the oscillation modes additionally reveals the stellar spin axis to be nearly edge-on, which suggests that the stellar spin is likely well aligned with the orbit of the transiting planet. The host star exhibits high signal-to-noise ratio asteroseismic oscillations, which enable precise measurements of the stellar mass, radius, and age. We report the discovery of Kepler-432b, a giant planet ( 87), faint companion ( Kepler-432B) that is a physically bound M dwarf. Christensen-Dalsgaard, Jørgen Elsworth, Yvonne P. Hekker, Saskia Kjeldsen, Hans Kuszlewicz, James S. Jiang, Chen Silva Aguirre, Victor Stello, Dennis Sliski, David H. Handberg, Rasmus Huber, Daniel Kipping, David M. Kepler-432: A Red Giant Interacting with One of its Two Long-period Giant Planets
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