Stellar Ages of M Dwarf Hosts of Temperate Sub-Neptunes

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ID: 328002
2026
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Abstract
Abstract Measuring the ages of M dwarfs remains one of the central Measuring M dwarf ages is a central challenge in stellar astrophysics. These stars evolve so slowly that isochrone fitting gives little constraint, requiring alternative methods based on rotation, activity, and kinematics. Reliable ages help constrain the formation and evolution of planetary systems around M dwarfs, including the temperate sub-Neptunes now being characterised with the James Webb Space Telescope (JWST). We present an age analysis of six nearby M dwarf planet hosts (TOI-732, TOI-736, TOI-270, TOI-1468, TOI-1231, and K2-18) using lithium absorption at 6708,Å, rotation periods, and Galactic kinematics. The Li I 6708,Å feature is absent above 3σ in all targets, implying substantial depletion and ages exceeding 200 Myr. Rotation periods of 39–145 days yield ages of 2.8–8.6 Gyr, calibrated against open cluster M dwarfs and including the intrinsic dispersion of the rotation–age relation. Kinematic ages span 0.8–13 Gyr with uncertainties of 4–6 Gyr. These are less precise per star but help identify outliers such as TOI-1231 (~13 Gyr) and K2-18 ( ~1–2 Gyr) and place the stars in Galactic context. Rotation yields age constraints 2–6 times tighter than kinematics where periods are measured, and comparable constraints where periods must be inferred from chromospheric activity. Combining multiple indicators enables more secure classification of these stars’ evolutionary states, providing reference points for future comparative studies.
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Authors S. Lalitha, Nikku Madhusudhan
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1635
URL
https://doi.org/10.1093/mnras/stag1635
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