Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 920, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/2041-8213/ac2600
Keywords
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Categories
Funding
- Pennsylvania State University
- Eberly College of Science
- NOIRLab through the Mid-Scale Innovations Program
- NSF
- NOIRLab program [2021A0147]
- DPAC
- NASA's Science Mission directorate
- NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center
- European Research Council (ERC) under the European Union [803193/BEBOP]
- Science and Technology Facilities Council (STFC) [ST/S00193X/1]
- French and Italian polar agencies IPEV
- PNRA [ANR-15-IDEX-01]
- Australian Research Council LIEF [LE160100001, DP180100972]
- Mount Cuba Astronomical Foundation
- institutional partners University of Southern Queensland
- UNSW Sydney
- MIT
- Nanjing University
- George Mason University
- University of Louisville
- University of California Riverside
- University of Florida
- University of Texas at Austin
- NASA XRP [80NSSC18K0355]
- NASA TESS [80NSSC18K1695]
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High-eccentricity tidal migration is a potential mechanism for placing giant planets in short-period orbits. TOI-3362b, a planet with a highly eccentric orbit, is believed to be undergoing high-eccentricity tidal migration. Follow-up observations of the system are needed to test various hypotheses explaining the extreme eccentricity of the planet's orbit.
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 M (Jup) 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 -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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