Stellar and Planetary Characterization of the Ross 128 Exoplanetary System from APOGEE Spectra

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dc.contributor.authorSouto, Diogo
dc.contributor.authorUnterborn, Cayman T.
dc.contributor.authorSmith, Verne V.
dc.contributor.authorCunha, Katia
dc.contributor.authorTeske, Johanna
dc.contributor.authorCovey, Kevin
dc.contributor.authorRojas-Ayala, Bárbara
dc.contributor.authorGarcía-Hernández D.A.
dc.contributor.authorStassun, Keivank, I.
dc.contributor.authorZamora, Olga
dc.contributor.authorMasseron, Thomas
dc.contributor.authorJohnson J.A.
dc.contributor.authorMajewski, Steven R.
dc.contributor.authorJönsson, Henrik
dc.contributor.authorGilhool, Steven
dc.contributor.authorBlake, Cullen
dc.contributor.authorSantana, Felipe
dc.date.accessioned2022-07-29T22:58:38Z
dc.date.available2022-07-29T22:58:38Z
dc.date.issued2018-06
dc.descriptionIndexación Scopuses
dc.description.abstractThe first detailed chemical abundance analysis of the M-dwarf (M4.0) exoplanet-hosting star Ross 128 is presented here, based upon near-infrared (1.5-1.7 μm), high-resolution (R ∼ 22,500) spectra from the SDSS Apache Point Galactic Evolution Experiment survey. We determined precise atmospheric parameters T eff = 3231 ±100 K, log g = 4.96 ±0.11 dex and chemical abundances of eight elements (C, O, Mg, Al, K, Ca, Ti, and Fe), finding Ross 128 to have near solar metallicity ([Fe/H] = +0.03 ± 0.09 dex). The derived results were obtained via spectral synthesis (1D LTE) adopting both MARCS and PHOENIX model atmospheres; stellar parameters and chemical abundances derived from the different adopted models do not show significant offsets. Mass-radius modeling of Ross 128b indicates that it lies below the pure-rock composition curve, suggesting that it contains a mixture of rock and iron, with the relative amounts of each set by the ratio of Fe/Mg. If Ross 128b formed with a subsolar Si abundance, and assuming the planet's composition matches that of the host star, it likely has a larger core size relative to the Earth despite this producing a planet with a Si/Mg abundance ratio ∼34% greater than the Sun. The derived planetary parameters - insolation flux (S Earth = 1.79 ±0.26) and equilibrium temperature (T eq = 294 ±10 K) - support previous findings that Ross 128b is a temperate exoplanet in the inner edge of the habitable zone. © 2018. The American Astronomical Society. All rights reserved.es
dc.description.urihttps://iopscience-iop-org.recursosbiblioteca.unab.cl/article/10.3847/2041-8213/aac896
dc.identifier.citationAstrophysical Journal Letters Volume 860, Issue 110 June 2018 Article number L15es
dc.identifier.doi10.3847/2041-8213/aac896
dc.identifier.issn20418205
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/23380
dc.language.isoenes
dc.publisherInstitute of Physics Publishinges
dc.rights.licenseCC BY 4.0
dc.subjectExoplanetses
dc.subjectKepleres
dc.subjectAtmospherees
dc.subjectplanetstar interactionses
dc.titleStellar and Planetary Characterization of the Ross 128 Exoplanetary System from APOGEE Spectraes
dc.typeArtículoes
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