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August 21, 2025Open Access

Metallicities of M Dwarf Planet Host Stars from Kepler, K2, and TESS Observed by APOGEE: Trends with Exoplanetary Radii and Orbital Periods

FWFábio WanderleyValongo Observatory KCKátia CunhaUniversity of Arizona DSDiogo SoutoUniversidade Federal de Sergipe

Key Points

Exoplanets with shorter orbital periods are found around more metal-rich stars, indicating a potential environmental influence.
Metal-rich stars host larger exoplanets, supporting the theory that larger planets form in metal-rich protoplanetary disks.
Using APOGEE data, stellar metallicities were derived, with trends observed in the distribution of planetary radii.
A distinct behavior is noted between single-detected exoplanets and those in multiplanetary systems, impacting metallicity associations.

Abstract

Abstract One important property in studying the exoplanet population is the host star metallicity (M/H). In this study, we derived stellar metallicities and oxygen abundances for 48 M dwarf stars using the near-infrared high-resolution spectra from the SDSS APOGEE survey and synthetic spectra computed in LTE. We also investigated the exoplanetary radii distribution for a larger sample of 246 exoplanets orbiting 188 M dwarf stars. The M/H versus O/M distribution obtained indicates that our sample is composed mainly of thin disk stars, which follow the behavior of the low-alpha sequence in the Milky Way thin disk. Small planets with radii smaller than 3 R ⊕ were found around stars with a range of metallicities (−0.6 4 R ⊕ shows a concentration at orbital periods between 2 and 5 days, which may result from inward orbital migration. There is also a different behavior between single-detected exoplanets and planets from multiplanetary systems, with the latter being found on average around more metal-poor stars, and with planetary radii roughly up to 3 R⊕.

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