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28 March 2024
 
  » arxiv » 1410.8114

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Planet Hunters VII. Discovery of a New Low-Mass, Low-Density Planet (PH3 c) Orbiting Kepler-289 with Mass Measurements of Two Additional Planets (PH3 b and d)
Joseph R. Schmitt ; Eric Agol ; Katherine M. Deck ; Leslie A. Rogers ; J. Zachary Gazak ; Debra A. Fischer ; Ji Wang ; Matthew J. Holman ; Kian J. Jek ; Charles Margossian ; Mark R. Omohundro ; Troy Winarski ; John M. Brewer ; Matthew J. Giguere ; Chris Lintott ; Stuart Lynn ; Michael Parrish ; Kevin Schawinski ; Megan E. Schwamb ; Robert Simpson ; Arfon M. Smith ;
Date 29 Oct 2014
AbstractWe report the discovery of one newly confirmed planet ($P=66.06$ days, $R_{ m{P}}=2.68pm0.17R_oplus$) and mass determinations of two previously validated Kepler planets, Kepler-289 b ($P=34.55$ days, $R_{ m{P}}=2.15pm0.10R_oplus$) and Kepler-289-c ($P=125.85$ days, $R_{ m{P}}=11.59pm0.10R_oplus$), through their transit timing variations (TTVs). We also exclude the possibility that these three planets reside in a $1:2:4$ Laplace resonance. The outer planet has very deep ($sim1.3%$), high signal-to-noise transits, which puts extremely tight constraints on its host star’s stellar properties via Kepler’s Third Law. The star PH3 is a young ($sim1$ Gyr as determined by isochrones and gyrochronology), Sun-like star with $M_*=1.08pm0.02M_odot$, $R_*=1.00pm0.02R_odot$, and $T_{ m{eff}}=5990pm38$ K. The middle planet’s large TTV amplitude ($sim5$ hours) resulted either in non-detections or inaccurate detections in previous searches. A strong chopping signal, a shorter period sinusoid in the TTVs, allows us to break the mass-eccentricity degeneracy and uniquely determine the masses of the inner, middle, and outer planets to be $M=7.3pm6.8M_oplus$, $4.0pm0.9M_oplus$, and $M=132pm17M_oplus$, which we designate PH3 b, c, and d, respectively. Furthermore, the middle planet, PH3 c, has a relatively low density, $ ho=1.2pm0.3$ g/cm$^3$ for a planet of its mass, requiring a substantial H/He atmosphere of $2.1^{+0.8}_{-0.3}%$ by mass, and joins a growing population of low-mass, low-density planets.
Source arXiv, 1410.8114
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