TOI-3362b: A Proto Hot Jupiter Undergoing High-eccentricity Tidal Migration

Dong, Jiayin and Huang, Chelsea X. ORCID: https://orcid.org/0000-0003-0918-7484 and Zhou, George ORCID: https://orcid.org/0000-0002-4891-3517 and Dawson, Rebekah I. and Rodriguez, Joseph E. and Eastman, Jason D. and Collins, Karen A. and Quinn, Samuel N. and Shporer, Avi and Triaud, Amaury H. M. J. and Wang, Songhu and Beatty, Thomas and Jackson, Jonathon M. and Collins, Kevin I. and Abe, Lyu and Suarez, Olga and Crouzet, Nicolas and Mekarnia, Djamel and Dransfield, Georgina and Jensen, Eric L. N. and Stockdale, Chris and Barkaoui, Khalid and Heitzmann, Alexis and Wright, Duncan J. ORCID: https://orcid.org/0000-0001-7294-5386 and Addison, Brett C. ORCID: https://orcid.org/0000-0003-3216-0626 and Wittenmyer, Robert A. and Okumura, Jack and Bowler, Brendan P. and Horner, Jonathan and Kane, Stephen R. and Kielkopf, John and Liu, Huigen and Plavchan, Peter and Mengel, Matthew W. ORCID: https://orcid.org/0000-0002-7830-6822 and Ricker, George R. and Vanderspek, Roland and Latham, David W. and Seager, S. and Winn, Joshua N. and Jenkins, Jon M. and Christiansen, Jessie L. and Paegert, Martin (2021) TOI-3362b: A Proto Hot Jupiter Undergoing High-eccentricity Tidal Migration. The Astrophysical Journal Letters, 920 (1):L16. pp. 1-11. ISSN 2041-8205

Text (Accepted Version) TOI3362b_arXiv.pdf Restricted - Available after 7 October 2022.

Abstract

High-eccentricity tidal migration is a possible way for giant planets to be placed in short-period orbits. If this happens often, one would expect to catch proto hot Jupiters on highly elliptical orbits undergoing high-eccentricity tidal migration. As of yet, few such systems have been discovered. Here, we introduce TOI-3362b (TIC-464300749b), an 18.1 day, 5 MJup planet orbiting a main-sequence F-type star that is likely undergoing high-eccentricity tidal migration. The orbital eccentricity is 0.815-0.032+0.023. With a semimajor axis of 0.153-0.003+0.002 au, the planet's orbit is expected to shrink to a final orbital radius of 0.051-0.006+0.008 au after complete tidal circularization. Several mechanisms could explain the extreme value of the planet's eccentricity, such as planet-planet scattering and secular interactions. Such hypotheses can be tested with follow-up observations of the system, e.g., measuring the stellar obliquity and searching for companions in the system with precise, long-term radial-velocity observations. The variation in the planet's equilibrium temperature as it orbits the host star and the tidal heating at periapse make this planet an intriguing target for atmospheric modeling and observation. Because the planet's orbital period of 18.1 days is near the limit of TESS's period sensitivity, even a few such discoveries suggest that proto hot Jupiters may be quite common.

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Item Type:	Article (Commonwealth Reporting Category C)
Refereed:	Yes
Item Status:	Live Archive
Faculty/School / Institute/Centre:	Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Faculty/School / Institute/Centre:	Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Date Deposited:	25 Jan 2022 00:43
Last Modified:	06 May 2022 02:45
Uncontrolled Keywords:	Exoplanet astronomy; Hot Jupiters; Transit photometry; Radial; velocity; Exoplanet migration; 486; 753; 1709; 1332; 2205; 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/10.3847/2041-8213/ac2600
URI:	http://eprints.usq.edu.au/id/eprint/44809

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