A planetary system with two transiting mini-Neptunes near the radius valley transition around the bright M dwarf TOI-776
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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 ± 0.03M⊙) 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 ofPb= 8.25 d, a radius ofRb= 1.85 ± 0.13R⊕, and a mass ofMb= 4.0 ± 0.9M⊕; and for the outer planet, TOI-776 c, a period ofPc= 15.66 d, a radius ofRc= 2.02 ± 0.14R⊕, and a mass ofMc= 5.3 ± 1.8M⊕. 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 0.54M⊙. Due to the brightness of the star, the TOI-776 system is also an excellent target for theJames WebbSpace 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.
