The Astronomical Journal (Jan 2023)

TOI-1136 is a Young, Coplanar, Aligned Planetary System in a Pristine Resonant Chain

  • Fei Dai,
  • Kento Masuda,
  • Corey Beard,
  • Paul Robertson,
  • Max Goldberg,
  • Konstantin Batygin,
  • Luke Bouma,
  • Jack J. Lissauer,
  • Emil Knudstrup,
  • Simon Albrecht,
  • Andrew W. Howard,
  • Heather A. Knutson,
  • Erik A. Petigura,
  • Lauren M. Weiss,
  • Howard Isaacson,
  • Martti Holst Kristiansen,
  • Hugh Osborn,
  • Songhu Wang,
  • Xian-Yu Wang,
  • Aida Behmard,
  • Michael Greklek-McKeon,
  • Shreyas Vissapragada,
  • Natalie M. Batalha,
  • Casey L. Brinkman,
  • Ashley Chontos,
  • Ian Crossfield,
  • Courtney Dressing,
  • Tara Fetherolf,
  • Benjamin Fulton,
  • Michelle L. Hill,
  • Daniel Huber,
  • Stephen R. Kane,
  • Jack Lubin,
  • Mason MacDougall,
  • Andrew Mayo,
  • Teo Močnik,
  • Joseph M. Akana Murphy,
  • Ryan A. Rubenzahl,
  • Nicholas Scarsdale,
  • Dakotah Tyler,
  • Judah Van Zandt,
  • Alex S. Polanski,
  • Hans Martin Schwengeler,
  • Ivan A. Terentev,
  • Paul Benni,
  • Allyson Bieryla,
  • David Ciardi,
  • Ben Falk,
  • E. Furlan,
  • Eric Girardin,
  • Pere Guerra,
  • Katharine M. Hesse,
  • Steve B. Howell,
  • J. Lillo-Box,
  • Elisabeth C. Matthews,
  • Joseph D. Twicken,
  • Joel Villaseñor,
  • David W. Latham,
  • Jon M. Jenkins,
  • George R. Ricker,
  • Sara Seager,
  • Roland Vanderspek,
  • Joshua N. Winn

DOI
https://doi.org/10.3847/1538-3881/aca327
Journal volume & issue
Vol. 165, no. 2
p. 33

Abstract

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Convergent disk migration has long been suspected to be responsible for forming planetary systems with a chain of mean-motion resonances (MMRs). Dynamical evolution over time could disrupt the delicate resonant configuration. We present TOI-1136, a 700 ± 150 Myr old G star hosting at least six transiting planets between ∼2 and 5 R _⊕ . The orbital period ratios deviate from exact commensurability by only 10 ^−4 , smaller than the ∼10 ^−2 deviations seen in typical Kepler near-resonant systems. A transit-timing analysis measured the masses of the planets (3–8 M _⊕ ) and demonstrated that the planets in TOI-1136 are in true resonances with librating resonant angles. Based on a Rossiter–McLaughlin measurement of planet d, the star’s rotation appears to be aligned with the planetary orbital planes. The well-aligned planetary system and the lack of a detected binary companion together suggest that TOI-1136's resonant chain formed in an isolated, quiescent disk with no stellar flyby, disk warp, or significant axial asymmetry. With period ratios near 3:2, 2:1, 3:2, 7:5, and 3:2, TOI-1136 is the first known resonant chain involving a second-order MMR (7:5) between two first-order MMRs. The formation of the delicate 7:5 resonance places strong constraints on the system’s migration history. Short-scale (starting from ∼0.1 au) Type-I migration with an inner disk edge is most consistent with the formation of TOI-1136. A low disk surface density (Σ _1 au ≲ 10 ^3 g cm ^−2 ; lower than the minimum-mass solar nebula) and the resultant slower migration rate likely facilitated the formation of the 7:5 second-order MMR.

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