A transiting giant planet in orbit around a 0.2-solar-mass host star

IF 12.9 1区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Nature Astronomy Pub Date : 2025-06-04 DOI:10.1038/s41550-025-02552-4

Edward M. Bryant, Andrés Jordán, Joel D. Hartman, Daniel Bayliss, Elyar Sedaghati, Khalid Barkaoui, Jamila Chouqar, Francisco J. Pozuelos, Daniel P. Thorngren, Mathilde Timmermans, Jose Manuel Almenara, Igor V. Chilingarian, Karen A. Collins, Tianjun Gan, Steve B. Howell, Norio Narita, Enric Palle, Benjamin V. Rackham, Amaury H. M. J. Triaud, Gaspar Á. Bakos, Rafael Brahm, Melissa J. Hobson, Vincent Van Eylen, Pedro J. Amado, Luc Arnold, Xavier Bonfils, Artem Burdanov, Charles Cadieux, Douglas A. Caldwell, Victor Casanova, David Charbonneau, Catherine A. Clark, Kevin I. Collins, Tansu Daylan, Georgina Dransfield, Brice-Olivier Demory, Elsa Ducrot, Gareb Fernández-Rodríguez, Izuru Fukuda, Akihiko Fukui, Michaël Gillon, Rebecca Gore, Matthew J. Hooton, Kai Ikuta, Emmanuel Jehin, Jon M. Jenkins, Alan M. Levine, Colin Littlefield, Felipe Murgas, Kendra Nguyen, Hannu Parviainen, Didier Queloz, S. Seager, Daniel Sebastian, Gregor Srdoc, R. Vanderspek, Joshua N. Winn, Julien de Wit, Sebastián Zúñiga-Fernández

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Abstract

Planet formation models indicate that the formation of giant planets is substantially harder around low-mass stars due to the scaling of protoplanetary disc masses with stellar mass. The discovery of giant planets orbiting such low-mass stars thus imposes strong constraints on giant planet formation processes. Here we report the discovery of a transiting giant planet orbiting a 0.207 ± 0.011 M_⊙ star. The planet, TOI-6894 b, has a mass and radius of M_P = 0.168 ± 0.022 M_J (53.4 ± 7.1 M_⊕) and R_P = 0.855 ± 0.022 R_J and probably includes 12 ± 2 M_⊕ of metals. The discovery of TOI-6894 b highlights the need for a better understanding of giant planet formation mechanisms and the protoplanetary disc environments in which they occur. The extremely deep transits (17% depth) make TOI-6894 b one of the most accessible exoplanetary giants for atmospheric characterization observations, which will be key for fully interpreting the formation history of this notable system and for the study of atmospheric methane chemistry.

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一颗围绕0.2太阳质量的主星运行的凌日巨行星

行星形成模型表明，由于原行星盘质量与恒星质量的比例关系，在低质量恒星周围形成巨行星要困难得多。围绕如此低质量恒星运行的巨行星的发现，因此对巨行星的形成过程施加了强烈的限制。在这里，我们报告发现了一颗绕0.207±0.011 M⊙恒星运行的凌日巨行星。这颗行星TOI-6894 b的质量和半径为MP = 0.168±0.022 MJ(53.4±7.1 M⊕),RP = 0.855±0.022 RJ，可能含有12±2 M⊕的金属。TOI-6894 b的发现强调了更好地理解巨行星形成机制和它们发生的原行星盘环境的必要性。极深的凌日（17%的深度）使TOI-6894 b成为大气特征观测最容易接近的系外行星之一，这将是全面解释这个著名系统的形成历史和研究大气甲烷化学的关键。

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来源期刊

Nature Astronomy Physics and Astronomy-Astronomy and Astrophysics

CiteScore

19.50

自引率

2.80%

发文量

252

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