학술논문
A massive hot Jupiter orbiting a metal-rich early-M star discovered in the TESS full frame images
Document Type
Working Paper
Author
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.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Burdanov, Artem; Charbonneau, David; Dransfield, Georgina; Fukui, Akihiko; Furlan, Elise; Gillon, Michaël; Hooton, Matthew J.; Lewis, Hannah M.; Littlefield, Colin; Mireles, Ismael; Narita, Norio; Ormel, Chris W.; Quinn, Samuel N.; Sefako, Ramotholo; Timmermans, Mathilde; Vezie, Michael; de Wit, Julien
Source
Subject
Language
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 remains 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 $1.22\pm 0.04\ R_J$ and a mass of $2.48\pm0.09\ M_J$, about 5 times heavier than most other giant planets around M dwarfs. It also has the highest planet-to-star mass ratio ($q\sim 4\times 10^{-3}$) among such systems. The host star is an early-M dwarf with a mass of $0.61\pm0.02\ M_{\odot}$ and a radius of $0.63\pm0.02\ R_{\odot}$. It has significant super-solar iron abundance ([Fe/H]=$0.52\pm 0.08$ 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.
Comment: 24 pages, 14 figures, 4 tables, accepted to AJ
Comment: 24 pages, 14 figures, 4 tables, accepted to AJ