Dynamics and Formation of the Near-resonant K2-24 System: Insights from Transit-timing Variations and Radial Velocities

• Published in: The Astronomical journal Vol. 156; no. 3; pp. 89 - 100
• Main Authors: Petigura, Erik A., Benneke, Björn, Batygin, Konstantin, Fulton, Benjamin J., Werner, Michael, Krick, Jessica E., Gorjian, Varoujan, Sinukoff, Evan, Deck, Katherine M., Mills, Sean M., Deming, Drake
• Format: Journal Article
• Language: English
• Published: Madison The American Astronomical Society 01.09.2018; IOP Publishing
• Subjects: Accretion; Astronomy; Deposition; Eccentricity; Orbital resonances (celestial mechanics); Orbits; Planets; planets and satellites: dynamical evolution and stability; planets and satellites: formation; planets and satellites: individual (K2-24b,K2-24c); Protoplanetary disks; Radial velocity; Solar system; techniques: radial velocities; Transit; Uranus
• ISSN: 0004-6256; 1538-3881
• DOI: 10.3847/1538-3881/aaceac

While planets between the size of Uranus and Saturn are absent within the solar system, the star K2-24 hosts two such planets, K2-24b and c, with radii equal to 5.4 and 7.5 , respectively. The two planets have orbital periods of 20.9 days and 42.4 days, residing only 1% outside the nominal 2:1 mean-motion resonance. In this work, we present results from a coordinated observing campaign to measure planet masses and eccentricities that combines radial velocity measurements from Keck/HIRES and transit-timing measurements from K2 and Spitzer. K2-24b and c have low, but nonzero, eccentricities of . The low observed eccentricities provide clues to the formation and dynamical evolution of K2-24b and K2-24c, suggesting that they could be the result of stochastic gravitational interactions with a turbulent protoplanetary disk, among other mechanisms. K2-24b and c are and , respectively; K2-24c is 20% less massive than K2-24b, despite being 40% larger. Their large sizes and low masses imply large envelope fractions, which we estimate at % and %. In particular, K2-24c's large envelope presents an intriguing challenge to the standard model of core-nucleated accretion that predicts the onset of runaway accretion when 50%.