Details

Autor(en) / Beteiligte

• 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
• Akana Murphy, Joseph M.
• Rubenzahl, Ryan A.
• Scarsdale, Nicholas
• Tyler, Dakotah
• Zandt, Judah Van
• 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.

Titel

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

Ist Teil von

• The Astronomical journal, 2023-02, Vol.165 (2), p.33

Ort / Verlag

Madison: The American Astronomical Society

Erscheinungsjahr

2023

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• Abstract 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.