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TOI-1136 is a Young, Coplanar, Aligned Planetary System in a Pristine Resonant Chain
- Source :
- Dai, F, Masuda, K, Beard, C, Robertson, P, Goldberg, M, Batygin, K, Bouma, L, Lissauer, J J, Knudstrup, E, Albrecht, S, Howard, A W, Knutson, H A, Petigura, E A, Weiss, L M, Isaacson, H, Kristiansen, M H, Osborn, H, Wang, S, Wang, X Y, Behmard, A, Greklek-McKeon, M, Vissapragada, S, Batalha, N M, Brinkman, C L, Chontos, A, Crossfield, I, Dressing, C, Fetherolf, T, Fulton, B, Hill, M L, Huber, D, Kane, S R, Lubin, J, MacDougall, M, Mayo, A, Močnik, T, Akana Murphy, J M, Rubenzahl, R A, Scarsdale, N, Tyler, D, Zandt, J V, Polanski, A S, Schwengeler, H M, Terentev, I A, Benni, P, Bieryla, A, Ciardi, D, Falk, B, Furlan, E, Girardin, E, Guerra, P, Hesse, K M, Howell, S B, Lillo-Box, J, Matthews, E C, Twicken, J D, Villaseñor, J, Latham, D W, Jenkins, J M, Ricker, G R, Seager, S, Vanderspek, R & Winn, J N 2023, ' TOI-1136 is a Young, Coplanar, Aligned Planetary System in a Pristine Resonant Chain ', Astronomical Journal, vol. 165, no. 2, 33 . https://doi.org/10.3847/1538-3881/aca327
- Publication Year :
- 2022
- Publisher :
- arXiv, 2022.
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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.<br />Comment: 48 pages, 23 figures, 8 tables. Accepted to AAS journals. Comments welcome!
Details
- Database :
- OpenAIRE
- Journal :
- Dai, F, Masuda, K, Beard, C, Robertson, P, Goldberg, M, Batygin, K, Bouma, L, Lissauer, J J, Knudstrup, E, Albrecht, S, Howard, A W, Knutson, H A, Petigura, E A, Weiss, L M, Isaacson, H, Kristiansen, M H, Osborn, H, Wang, S, Wang, X Y, Behmard, A, Greklek-McKeon, M, Vissapragada, S, Batalha, N M, Brinkman, C L, Chontos, A, Crossfield, I, Dressing, C, Fetherolf, T, Fulton, B, Hill, M L, Huber, D, Kane, S R, Lubin, J, MacDougall, M, Mayo, A, Močnik, T, Akana Murphy, J M, Rubenzahl, R A, Scarsdale, N, Tyler, D, Zandt, J V, Polanski, A S, Schwengeler, H M, Terentev, I A, Benni, P, Bieryla, A, Ciardi, D, Falk, B, Furlan, E, Girardin, E, Guerra, P, Hesse, K M, Howell, S B, Lillo-Box, J, Matthews, E C, Twicken, J D, Villaseñor, J, Latham, D W, Jenkins, J M, Ricker, G R, Seager, S, Vanderspek, R & Winn, J N 2023, ' TOI-1136 is a Young, Coplanar, Aligned Planetary System in a Pristine Resonant Chain ', Astronomical Journal, vol. 165, no. 2, 33 . https://doi.org/10.3847/1538-3881/aca327
- Accession number :
- edsair.doi.dedup.....5bf859603a6d096a88365c8c2c5ef8d1
- Full Text :
- https://doi.org/10.48550/arxiv.2210.09283