The Astronomical Journal (Jan 2023)

A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images

  • Tianjun Gan,
  • Charles Cadieux,
  • Farbod Jahandar,
  • Allona Vazan,
  • Sharon X. Wang,
  • Shude Mao,
  • Jaime A. Alvarado-Montes,
  • D. N. C. Lin,
  • Étienne Artigau,
  • Neil J. Cook,
  • René Doyon,
  • Andrew W. Mann,
  • Keivan G. Stassun,
  • Adam J. Burgasser,
  • Benjamin V. Rackham,
  • Steve B. Howell,
  • Karen A. Collins,
  • Khalid Barkaoui,
  • Avi Shporer,
  • Jerome de Leon,
  • Luc Arnold,
  • George R. Ricker,
  • Roland Vanderspek,
  • David W. Latham,
  • Sara Seager,
  • Joshua N. Winn,
  • Jon M. Jenkins,
  • Artem Burdanov,
  • David Charbonneau,
  • Georgina Dransfield,
  • Akihiko Fukui,
  • Elise Furlan,
  • Michaël Gillon,
  • Matthew J. Hooton,
  • Hannah M. Lewis,
  • Colin Littlefield,
  • Ismael Mireles,
  • Norio Narita,
  • Chris W. Ormel,
  • Samuel N. Quinn,
  • Ramotholo Sefako,
  • Mathilde Timmermans,
  • Michael Vezie,
  • Julien de Wit

DOI
https://doi.org/10.3847/1538-3881/acf56d
Journal volume & issue
Vol. 166, no. 4
p. 165

Abstract

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Observations and statistical studies have shown that giant planets are rare around M dwarfs compared with Sun-like stars. The formation mechanism of these extreme systems has remained under debate for decades. With the help of the TESS mission and ground-based follow-up observations, we report the discovery of TOI-4201b, the most massive and densest hot Jupiter around an M dwarf known so far with a radius of 1.22 ± 0.04 R _J and a mass of 2.48 ± 0.09 M _J , about 5 times heavier than most other giant planets around M dwarfs. It also has the highest planet-to-star mass ratio ( q ∼ 4 × 10 ^−3 ) among such systems. The host star is an early M dwarf with a mass of 0.61 ± 0.02 M _⊙ and a radius of 0.63 ± 0.02 R _⊙ . It has significant supersolar iron abundance ([Fe/H] = 0.52 ± 0.08 dex). However, interior structure modeling suggests that its planet TOI-4201b is metal-poor, which challenges the classical core-accretion correlation of stellar−planet metallicity, unless the planet is inflated by additional energy sources. Building on the detection of this planet, we compare the stellar metallicity distribution of four planetary groups: hot/warm Jupiters around G/M dwarfs. We find that hot/warm Jupiters show a similar metallicity dependence around G-type stars. For M-dwarf host stars, the occurrence of hot Jupiters shows a much stronger correlation with iron abundance, while warm Jupiters display a weaker preference, indicating possible different formation histories.

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