Stellar Characterization and Radius Inflation of Hyades M-dwarf Stars from the APOGEE Survey

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dc.contributor.authorWanderley, Fábio
dc.contributor.authorCunha, Katia
dc.contributor.authorSouto, Diogo
dc.contributor.authorSmith, Verne V.
dc.contributor.authorCao, Lyra
dc.contributor.authorPinsonneault, Marc
dc.contributor.authorAllende Prieto, C.
dc.contributor.authorCovey, Kevin
dc.contributor.authorMasseron, Thomas
dc.contributor.authorPascucci, Ilaria
dc.contributor.authorStassun, Keivan G.
dc.contributor.authorTerrien, Ryan
dc.contributor.authorBergsten, Galen J.
dc.contributor.authorBizyaev, Dmitry
dc.contributor.authorFernández-Trincado, José G.
dc.contributor.authorJönsson, Henrik
dc.contributor.authorHasselquist, Sten
dc.contributor.authorHoltzman, Jon A.
dc.contributor.authorLane, Richard R.
dc.contributor.authorMahadevan, Suvrath
dc.contributor.authorMajewski, Steven R.
dc.contributor.authorMinniti, Dante
dc.contributor.authorPan, Kaike
dc.contributor.authorSerna, Javier
dc.contributor.authorSobeck, Jennifer
dc.contributor.authorStringfellow, Guy S.
dc.date.accessioned2023-11-03T12:04:02Z
dc.date.available2023-11-03T12:04:02Z
dc.date.issued2023-07-01
dc.descriptionIndexación: Scopuses
dc.description.abstractWe present a spectroscopic analysis of a sample of 48 M-dwarf stars (0.2 M ⊙ < M < 0.6 M ⊙) from the Hyades open cluster using high-resolution H-band spectra from the Sloan Digital Sky Survey/Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. Our methodology adopts spectrum synthesis with LTE MARCS model atmospheres, along with the APOGEE Data Release 17 line list, to determine effective temperatures, surface gravities, metallicities, and projected rotational velocities. The median metallicity obtained for the Hyades M dwarfs is [M/H] = 0.09 ± 0.03 dex, indicating a small internal uncertainty and good agreement with optical results for Hyades red giants. Overall, the median radii are larger than predicted by stellar models by 1.6% ± 2.3% and 2.4% ± 2.3%, relative to a MIST and DARTMOUTH isochrone, respectively. We emphasize, however, that these isochrones are different, and the fractional radius inflation for the fully and partially convective regimes have distinct behaviors depending on the isochrone. Using a MIST isochrone there is no evidence of radius inflation for the fully convective stars, while for the partially convective M dwarfs the radii are inflated by 2.7% ± 2.1%, which is in agreement with predictions from models that include magnetic fields. For the partially convective stars, rapid rotators present on average higher inflation levels than slow rotators. The comparison with SPOTS isochrone models indicates that the derived M-dwarf radii can be explained by accounting for stellar spots in the photosphere of the stars, with 76% of the studied M dwarfs having up to 20% spot coverage, and the most inflated stars with ∼20%-40% spot coverage.es
dc.identifier.citationAstrophysical Journal Volume 951, Issue 2 1 July 2023 Article number 90es
dc.identifier.doi10.3847/1538-4357/acd4bden
dc.identifier.issn0004-637X
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/53810
dc.language.isoenes
dc.publisherInstitute of Physicses
dc.rights.licenseCC BY 4.0 DEED Atribución 4.0 Internacionalen
dc.subjectDwarfismes
dc.subjectColor-Magnitude Diagrames
dc.subjectWide-Field Infrared Survey Exploreres
dc.titleStellar Characterization and Radius Inflation of Hyades M-dwarf Stars from the APOGEE Surveyes
dc.typeArtículoes
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