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

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

doi:10.3847/1538-3881/aca327

Cited by 29 publications

(15 citation statements)

References 205 publications

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“…However, f ¢ 1 and f ¢ 2 are now in circulation, so an analysis which only computed these angles would classify this system as "nonresonant." In general, TTV fits cannot distinguish between these two configurations (Leleu et al 2021) and therefore they frequently recover both librating and circulating solutions to the same data, even if ψ librates across nearly all of the allowed entire parameter space (Dai et al 2023).…”

Section: Aside: Pitfalls Of Determining Libration With Standard Reson...mentioning

confidence: 99%

Dynamics and Origins of the Near-resonant Kepler Planets

Goldberg

Batygin

2023

ApJ

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Short-period super-Earths and mini-Neptunes encircle more than ∼50% of Sun-like stars and are relatively amenable to direct observational characterization. Despite this, environments in which these planets accrete are difficult to probe directly. Nevertheless, pairs of planets that are close to orbital resonances provide a unique window into the inner regions of protoplanetary disks, as they preserve the conditions of their formation, as well as the early evolution of their orbital architectures. In this work, we present a novel approach toward quantifying transit timing variations within multiplanetary systems and examine the near-resonant dynamics of over 100 planet pairs detected by Kepler. Using an integrable model for first-order resonances, we find a clear transition from libration to circulation of the resonant angle at a period ratio of ≈0.6% wide of exact resonance. The orbital properties of these systems indicate that they systematically lie far away from the resonant forced equilibrium. Cumulatively, our modeling indicates that while orbital architectures shaped by strong disk damping or tidal dissipation are inconsistent with observations, a scenario where stochastic stirring by turbulent eddies augments the dissipative effects of protoplanetary disks reproduces several features of the data.

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Section: Aside: Pitfalls Of Determining Libration With Standard Reson...mentioning

confidence: 99%

Dynamics and Origins of the Near-resonant Kepler Planets

Goldberg

Batygin

2023

ApJ

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“…Therefore, an appealing formation scenario for the compact TOI-2076 b system is through smooth disk migration within an initially well-aligned protoplanetary disk (e.g., Goldreich & Tremaine 1979, 1980, where the planets migrated into their resonant orbits that we see today. Future RM effect observations of TOI-2076 c and d will help constrain the coplanarity of the system, which through these lines of evidence we would expect to be likely wellaligned with the orbit of planet b. TOI-2076 b is similar to the recently studied TOI-1136 system (Dai et al 2023), which is a compact network of at least six transiting planets in a resonant chain that likely formed through smooth disk migration in an initially well-aligned disk.…”

Section: Obliquities As a Function Of Agementioning

confidence: 67%

NEID Reveals That the Young Warm Neptune TOI-2076 b Has a Low Obliquity

Frazier

Stefánsson

Mahadevan

et al. 2023

ApJL

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TOI-2076 b is a sub-Neptune-sized planet (R = 2.39 ± 0.10 R ⊕) that transits a young (204 ± 50 MYr) bright (V = 9.2) K-dwarf hosting a system of three transiting planets. Using spectroscopic observations obtained with the NEID spectrograph on the WIYN 3.5 m Telescope, we model the Rossiter–McLaughlin effect of TOI-2076 b, and derive a sky-projected obliquity of λ = − 3 − 15 + 16 ° . Using the size of the star (R = 0.775 ± 0.015 R ⊙), and the stellar rotation period (P rot = 7.27 ± 0.23 days), we estimate an obliquity of ψ = 18 − 9 + 10 ° (ψ < 34° at 95% confidence), demonstrating that TOI-2076 b is in a well-aligned orbit. Simultaneous diffuser-assisted photometry from the 3.5 m telescope at Apache Point Observatory rules out flares during the transit. TOI-2076 b joins a small but growing sample of young planets in compact multi-planet systems with well-aligned orbits, and is the fourth planet with an age ≲300 Myr in a multi-transiting system with an obliquity measurement. The low obliquity of TOI-2076 b and the presence of transit timing variations in the system suggest the TOI-2076 system likely formed via convergent disk migration in an initially well-aligned disk.

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“…(3) circulate, so long as the mixed angle still librates. An example of a multiplanet system where this occurs is given in Dai et al (2023), and the planets in this system appear to be in both three-body and two-body MMR despite Equations (2) and…”

Section: Two-body Resonancesmentioning

confidence: 99%

Kepler-80 Revisited: Assessing the Participation of a Newly Discovered Planet in the Resonant Chain

Weisserman

Becker

Vanderburg

2023

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In this paper, we consider the chain of resonances in the Kepler-80 system and evaluate the impact that the additional member of the resonant chain discovered by Shallue & Vanderburg has on the dynamics of the system and the physical parameters that can be recovered by a fit to the transit timing variations (TTVs). Ultimately, we calculate the mass of Kepler-80 g to be 0.8 ± 0.3M ⊕ when assuming all planets have zero eccentricity, and 1.0 ± 0.3 M ⊕ when relaxing that assumption. We show that the outer five planets are in successive three-body mean-motion resonances (MMRs). We assess the current state of two-body MMRs in the system and find that the planets do not appear to be in two-body MMRs. We find that while the existence of the additional member of the resonant chain does not significantly alter the character of the Kepler-80 three-body MMRs, it can alter the physical parameters derived from the TTVs, suggesting caution should be applied when drawing conclusions from TTVs for potentially incomplete systems. We also compare our results to those of MacDonald et al., who perform a similar analysis on the same system with a different method. Although the results of this work and MacDonald et al. show that different fit methodologies and underlying assumptions can result in different measured orbital parameters, the most secure conclusion is that which holds true across all lines of analysis: Kepler-80 contains a chain of planets in three-body MMRs but not in two-body MMRs.

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

Cited by 29 publications

References 205 publications

Dynamics and Origins of the Near-resonant Kepler Planets

Dynamics and Origins of the Near-resonant Kepler Planets

NEID Reveals That the Young Warm Neptune TOI-2076 b Has a Low Obliquity

Kepler-80 Revisited: Assessing the Participation of a Newly Discovered Planet in the Resonant Chain

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