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

Author:

Gan TianjunORCID,Cadieux CharlesORCID,Jahandar FarbodORCID,Vazan AllonaORCID,Wang Sharon X.ORCID,Mao ShudeORCID,Alvarado-Montes Jaime A.ORCID,Lin D. N. C.ORCID,Artigau ÉtienneORCID,Cook Neil J.ORCID,Doyon RenéORCID,Mann Andrew W.ORCID,Stassun Keivan G.ORCID,Burgasser Adam J.ORCID,Rackham Benjamin V.ORCID,Howell Steve B.ORCID,Collins Karen A.ORCID,Barkaoui KhalidORCID,Shporer AviORCID,de Leon JeromeORCID,Arnold LucORCID,Ricker George R.ORCID,Vanderspek RolandORCID,Latham David W.ORCID,Seager SaraORCID,Winn Joshua N.ORCID,Jenkins Jon M.ORCID,Burdanov ArtemORCID,Charbonneau DavidORCID,Dransfield Georgina,Fukui AkihikoORCID,Furlan EliseORCID,Gillon MichaëlORCID,Hooton Matthew J.ORCID,Lewis Hannah M.ORCID,Littlefield ColinORCID,Mireles IsmaelORCID,Narita NorioORCID,Ormel Chris W.ORCID,Quinn Samuel N.ORCID,Sefako RamotholoORCID,Timmermans Mathilde,Vezie Michael,de Wit JulienORCID

Abstract

Abstract 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.

Funder

TESS Research Foundation

Publisher

American Astronomical Society

Subject

Space and Planetary Science,Astronomy and Astrophysics

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