Precise Transit and Radial-velocity Characterization of a Resonant Pair: The Warm Jupiter TOI-216c and Eccentric Warm Neptune TOI-216b

Dawson, Rebekah I. and Huang, Chelsea X. ORCID: https://orcid.org/0000-0003-0918-7484 and Brahm, Rafael and Collins, Karen A. and Hobson, Melissa J. and Jordan, Andres and Dong, Jiayin and Korth, Judith and Trifonov, Trifon and Abe, Lyu and Agabi, Abdelkrim and Bruni, Ivan and Butler, R. Paul and Barbieri, Mauro and Collins, Kevin I. and Conti, Dennis M. and Crane, Jeffrey D. and Crouzet, Nicolas and Dransfield, Georgina and Evans, Phil and Espinoza, Nestor and Gan, Tianjun and Guillot, Tristan and Henning, Thomas and Lissauer, Jack J. and Jensen, Eric L. N. and Marie Sainte, Wenceslas and Mekarnia, Djamel and Myers, Gordon and Nandakumar, Sangeetha and Relles, Howard M. and Sarkis, Paula and Torres, Pascal and Shectman, Stephen and Schmider, Francois-Xavier and Shporer, Avi and Stockdale, Chris and Teske, Johanna and Triaud, Amaury H. M. J. and Wang, Sharon Xuesong and Ziegler, Carl 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 Burt, Jennifer A. and Charbonneau, David and Levine, Alan M. and McDermott, Scott and McLean, Brian and Rose, Mark E. and Vanderburg, Andrew and Wohler, Bill (2021) Precise Transit and Radial-velocity Characterization of a Resonant Pair: The Warm Jupiter TOI-216c and Eccentric Warm Neptune TOI-216b. The Astronomical Journal, 161 (4):161. pp. 1-16. ISSN 0004-6256

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Abstract

TOI-216 hosts a pair of warm, large exoplanets discovered by the TESS mission. These planets were found to be in or near the 2:1 resonance, and both of them exhibit transit timing variations (TTVs). Precise characterization of the planets’ masses and radii, orbital properties, and resonant behavior can test theories for the origins of planets orbiting close to their stars. Previous characterization of the system using the first six sectors of TESS data suffered from a degeneracy between planet mass and orbital eccentricity. Radial-velocity measurements using HARPS, FEROS, and the Planet Finder Spectrograph break that degeneracy, and an expanded TTV baseline from TESS and an ongoing ground-based transit observing campaign increase the precision of the mass and eccentricity measurements. We determine that TOI-216c is a warm Jupiter, TOI-216b is an eccentric warm Neptune, and that they librate in 2:1 resonance with a moderate libration amplitude of 60-+22 deg, a small but significant free eccentricity of 0.0222-+0.00030.0005 for TOI-216b, and a small but significant mutual inclination of 1°.2–3°.9 (95% confidence interval). The libration amplitude, free eccentricity, and mutual inclination imply a disturbance of TOI-216b before or after resonance capture, perhaps by an undetected third planet.


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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Additional Information: Published version deposited in accordance with the copyright policy of the publisher.
Faculty/School / Institute/Centre: No Faculty
Faculty/School / Institute/Centre: No Faculty
Date Deposited: 03 Apr 2022 23:09
Last Modified: 09 Jun 2022 03:36
Uncontrolled Keywords: Exoplanet astronomy (486); Exoplanet dynamics (490); Transit timing variation method (1710); Radial velocity (1332); Astrophysics - Earth and Planetary Astrophysics
Fields of Research (2020): 51 PHYSICAL SCIENCES > 5101 Astronomical sciences > 510109 Stellar astronomy and planetary systems
Identification Number or DOI: https://doi.org/10.3847/1538-3881/abd8d0
URI: http://eprints.usq.edu.au/id/eprint/47427

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