TOI-216b and TOI-216 c: Two Warm, Large Exoplanets in or Slightly Wide of the 2:1 Orbital Resonance

Dawson, Rebekah I. and Huang, Chelsea X. ORCID: https://orcid.org/0000-0003-0918-7484 and Lissauer, Jack J. and Collins, Karen A. and Sha, Lizhou and Armstrong, James and Conti, Dennis M. and Collins, Kevin I. and Evans, Phil and Gan, Tianjun and Horne, Keith and Ireland, Michael and Murgas, Felipe and Myers, Gordon and Relles, Howard M. and Sefako, Ramotholo and Shporer, Avi and Stockdale, Chris and Zerjal, Marusa and Zhou, George ORCID: https://orcid.org/0000-0002-4891-3517 and Ricker, G. and Vanderspek, R. and Latham, David W. and Seager, S. and Winn, J. and Jenkins, Jon M. and Bouma, L. G. and Caldwell, Douglas A. and Daylan, Tansu and Doty, John P. and Dynes, Scott and Esquerdo, Gilbert A. and Rose, Mark and Smith, Jeffrey C. and Yu, Liang (2019) TOI-216b and TOI-216 c: Two Warm, Large Exoplanets in or Slightly Wide of the 2:1 Orbital Resonance. The Astronomical Journal, 158 (2):65. pp. 1-13. ISSN 0004-6256

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Abstract

Warm, large exoplanets with 10-100 day orbital periods pose a major challenge to our understanding of how planetary systems form and evolve. Although high eccentricity tidal migration has been invoked to explain their proximity to their host stars, a handful reside in or near orbital resonance with nearby planets, suggesting a gentler history of in situ formation or disk migration. Here we confirm and characterize a pair of warm, large exoplanets discovered by the TESS Mission orbiting K-dwarf TOI-216. Our analysis includes additional transits and transit exclusion windows observed via ground-based follow-up. We find two families of solutions, one corresponding to a sub-Saturn-mass planet accompanied by a Neptune-mass planet and the other to a Jupiter in resonance with a sub-Saturn-mass planet. We prefer the second solution based on the orbital period ratio, the planet radii, the lower free eccentricities, and libration of the 2:1 resonant argument, but cannot rule out the first. The free eccentricities and mutual inclination are compatible with stirring by other, undetected planets in the system, particularly for the second solution. We discuss prospects for better constraints on the planets’ properties and orbits through follow-up, including transits observed from the ground.


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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Faculty/School / Institute/Centre: No Faculty
Faculty/School / Institute/Centre: No Faculty
Date Deposited: 09 Feb 2022 04:06
Last Modified: 14 Feb 2022 01:04
Uncontrolled Keywords: planets and satellites: detection; planets and satellites: dynamical; evolution and stability; Astrophysics - Earth and Planetary Astrophysics
Fields of Research (2008): 02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems
Fields of Research (2020): 51 PHYSICAL SCIENCES > 5101 Astronomical sciences > 510109 Stellar astronomy and planetary systems
Socio-Economic Objectives (2008): E Expanding Knowledge > 97 Expanding Knowledge > 970102 Expanding Knowledge in the Physical Sciences
Socio-Economic Objectives (2020): 28 EXPANDING KNOWLEDGE > 2801 Expanding knowledge > 280120 Expanding knowledge in the physical sciences
Identification Number or DOI: https://doi.org/10.3847/1538-3881/ab24ba
URI: http://eprints.usq.edu.au/id/eprint/44984

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