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Gan, Tianjun; Cadieux, Charles; Jahandar, Farbod; Vazan, Allona; Wang, Sharon X.; Mao, Shude; Alvarado-Montes, Jaime A.; Lin, D. N. C.; Artigau, Étienne; Cook, Neil J.; Doyon, René; Mann, Andrew W.; Stassun, Keivan G.; Burgasser, Adam J.; Rackham, Benjamin V.; Howell, Steve B.; Collins, Karen A.; Barkaoui, Khalid; Shporer, Avi; de Leon, Jerome; Arnold, Luc; Ricker, George R.; Vanderspek, Roland; Latham, David W.; [...]

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

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  • Medientyp: E-Artikel
  • Titel: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
  • Beteiligte: Gan, Tianjun; Cadieux, Charles; Jahandar, Farbod; Vazan, Allona; Wang, Sharon X.; Mao, Shude; Alvarado-Montes, Jaime A.; Lin, D. N. C.; Artigau, Étienne; Cook, Neil J.; Doyon, René; Mann, Andrew W.; Stassun, Keivan G.; Burgasser, Adam J.; Rackham, Benjamin V.; Howell, Steve B.; Collins, Karen A.; Barkaoui, Khalid; Shporer, Avi; de Leon, Jerome; Arnold, Luc; Ricker, George R.; Vanderspek, Roland; Latham, David W.; [...]
  • Erschienen: American Astronomical Society, 2023
  • Erschienen in: The Astronomical Journal
  • Sprache: Nicht zu entscheiden
  • DOI: 10.3847/1538-3881/acf56d
  • ISSN: 1538-3881; 0004-6256
  • Schlagwörter: Space and Planetary Science ; Astronomy and Astrophysics
  • Entstehung:
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  • Beschreibung: <jats:title>Abstract</jats:title> <jats:p>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 <jats:italic>R</jats:italic> <jats:sub>J</jats:sub> and a mass of 2.48 ± 0.09 <jats:italic>M</jats:italic> <jats:sub>J</jats:sub>, about 5 times heavier than most other giant planets around M dwarfs. It also has the highest planet-to-star mass ratio (<jats:italic>q</jats:italic> ∼ 4 × 10<jats:sup>−3</jats:sup>) among such systems. The host star is an early M dwarf with a mass of 0.61 ± 0.02 <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub> and a radius of 0.63 ± 0.02 <jats:italic>R</jats:italic> <jats:sub>⊙</jats:sub>. 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.</jats:p>
  • Zugangsstatus: Freier Zugang