학술논문
TOI-1136 is a Young, Coplanar, Aligned Planetary System in a Pristine Resonant Chain
Document Type
Working Paper
Author
Dai, Fei; Masuda, Kento; Beard, Corey; Robertson, Paul; Goldberg, Max; Batygin, Konstantin; Bouma, Luke; Lissauer, Jack J.; Knudstrup, Emil; Albrecht, Simon; Howard, Andrew W.; Knutson, Heather A.; Petigura, Erik A.; Weiss, Lauren M.; Isaacson, Howard; Kristiansen, Martti Holst; Osborn, Hugh; Wang, Songhu; Wang, Xian-Yu; Behmard, Aida; Greklek-McKeon, Michael; Vissapragada, Shreyas; Batalha, Natalie M.; Brinkman, Casey L.; Chontos, Ashley; Crossfield, Ian; Dressing, Courtney; Fetherolf, Tara; Fulton, Benjamin; Hill, Michelle L.; Huber, Daniel; Kane, Stephen R.; Lubin, Jack; MacDougall, Mason; Mayo, Andrew; Močnik, Teo; Murphy, Joseph M. Akana; Rubenzahl, Ryan A.; Scarsdale, Nicholas; Tyler, Dakotah; Van Zandt, Judah; Polanski, Alex S.; Schwengeler, Hans Martin; Terentev, Ivan A.; Benni, Paul; Bieryla, Allyson; Ciardi, David; Falk, Ben; Furlan, E.; Girardin, Eric; Guerra, Pere; Hesse, Katharine M.; Howell, Steve B.; Lillo-Box, J.; Matthews, Elisabeth C.; Twicken, Joseph D.; Villaseñor, Joel; Latham, David W.; Jenkins, Jon M.; Ricker, George R.; Seager, Sara; Vanderspek, Roland; Winn, Joshua N.
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Subject
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Abstract
Convergent disk migration has long been suspected to be responsible for forming planetary systems with a chain of mean-motion resonances (MMR). Dynamical evolution over time could disrupt the delicate resonant configuration. We present TOI-1136, a 700-Myr-old G star hosting at least 6 transiting planets between $\sim$2 and 5 $R_\oplus$. The orbital period ratios deviate from exact commensurability by only $10^{-4}$, smaller than the $\sim$\,$10^{-2}$ deviations seen in typical Kepler near-resonant systems. A transit-timing analysis measured the masses of the planets (3-8$M_\oplus$) 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 detected binary companion together suggest that TOI-1136's resonant chain formed in an isolated, quiescent disk with no stellar fly-by, 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 MMR. The formation of the delicate 7:5 resonance places strong constraints on the system's migration history. Short-scale (starting from $\sim$0.1 AU) Type-I migration with an inner disk edge is most consistent with the formation of TOI-1136. A low disk surface density ($\Sigma_{\rm 1AU}\lesssim10^3$g~cm$^{-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. TOI-1136's deep resonance suggests that it has not undergone much resonant repulsion during its 700-Myr lifetime. One can rule out rapid tidal dissipation within a rocky planet b or obliquity tides within the largest planets d and f.
Comment: 48 pages, 23 figures, 8 tables. Accepted to AAS journals. Comments welcome!
Comment: 48 pages, 23 figures, 8 tables. Accepted to AAS journals. Comments welcome!