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Publication Detail
A planetary system with two transiting mini-Neptunes near the radius valley transition around the bright M dwarf TOI-776
  • Publication Type:
    Journal article
  • Publication Sub Type:
    Article
  • Authors:
    Luque R, Serrano LM, Molaverdikhani K, Nixon MC, Livingston JH, Guenther EW, Pallé E, Madhusudhan N, Nowak G, Korth J, Cochran WD, Hirano T, Chaturvedi P, Goffo E, Albrecht S, Barragán O, Briceño C, Cabrera J, Charbonneau D, Cloutier R, Collins KA, Collins KI, Colón KD, Crossfield IJM, Csizmadia S, Dai F, Deeg HJ, Esposito M, Fridlund M, Gandolfi D, Georgieva I, Glidden A, Goeke RF, Grziwa S, Hatzes AP, Henze CE, Howell SB, Irwin J, Jenkins JM, Jensen ELN, Kábath P, Kidwell RC, Kielkopf JF, Knudstrup E, Lam KWF, Latham DW, Lissauer JJ, Mann AW, Matthews EC, Mireles I, Narita N, Paegert M, Persson CM, Redfield S, Ricker GR, Rodler F, Schlieder JE, Scott NJ, Seager S, Šubjak J, Tan TG, Ting EB, Vanderspek R, Van Eylen V, Winn JN, Ziegler C
  • Publication date:
    05/01/2021
  • Journal:
    Astronomy and Astrophysics
  • Volume:
    645
  • Status:
    Published
  • Print ISSN:
    0004-6361
Abstract
© ESO 2021. We report the discovery and characterization of two transiting planets around the bright M1 V star LP 961-53 (TOI-776, J = 8.5 mag, M = 0.54 ± 0.03 M⊙) detected during Sector 10 observations of the Transiting Exoplanet Survey Satellite (TESS). Combining the TESS photometry with HARPS radial velocities, as well as ground-based follow-up transit observations from the MEarth and LCOGT telescopes, for the inner planet, TOI-776 b, we measured a period of Pb = 8.25 d, a radius of Rb = 1.85 ± 0.13 R⊙, and a mass of Mb = 4.0 ± 0.9 M⊙; and for the outer planet, TOI-776 c, a period of Pc = 15.66 d, a radius of Rc = 2.02 ± 0.14 R⊙, and a mass of Mc = 5.3 ± 1.8 M⊙. The Doppler data shows one additional signal, with a period of ~34 d, associated with the rotational period of the star. The analysis of fifteen years of ground-based photometric monitoring data and the inspection of different spectral line indicators confirm this assumption. The bulk densities of TOI-776 b and c allow for a wide range of possible interior and atmospheric compositions. However, both planets have retained a significant atmosphere, with slightly different envelope mass fractions. Thanks to their location near the radius gap for M dwarfs, we can start to explore the mechanism(s) responsible for the radius valley emergence around low-mass stars as compared to solar-like stars. While a larger sample of well-characterized planets in this parameter space is still needed to draw firm conclusions, we tentatively estimate that the stellar mass below which thermally-driven mass loss is no longer the main formation pathway for sculpting the radius valley is between 0.63 and 0.54 M⊙. Due to the brightness of the star, the TOI-776 system is also an excellent target for the James Webb Space Telescope, providing a remarkable laboratory in which to break the degeneracy in planetary interior models and to test formation and evolution theories of small planets around low-mass stars.
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