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Asteroseismic fundamental properties of solar-type stars observed by the NASA Kepler mission

Chaplin, W J; Basu, S; Huber, D; Serenelli, Aldo; Casagrande, Luca; Silva Aguirre, V; Ball, W.H.; Creevey, O L; Gizon, L; Handberg, R.; Karoff, C.

Description

We use asteroseismic data obtained by the NASA Kepler mission to estimate the fundamental properties of more than 500 main-sequence and sub-giant stars. Data obtained during the first 10 months of Kepler science operations were used for this work, when these solar-type targets were observed for one month each in survey mode. Stellar properties have been estimated using two global asteroseismic parameters and complementary photometric and spectroscopic data. Homogeneous sets of effective...[Show more]

dc.contributor.authorChaplin, W J
dc.contributor.authorBasu, S
dc.contributor.authorHuber, D
dc.contributor.authorSerenelli, Aldo
dc.contributor.authorCasagrande, Luca
dc.contributor.authorSilva Aguirre, V
dc.contributor.authorBall, W.H.
dc.contributor.authorCreevey, O L
dc.contributor.authorGizon, L
dc.contributor.authorHandberg, R.
dc.contributor.authorKaroff, C.
dc.date.accessioned2015-12-10T23:32:28Z
dc.identifier.issn0067-0049
dc.identifier.urihttp://hdl.handle.net/1885/68852
dc.description.abstractWe use asteroseismic data obtained by the NASA Kepler mission to estimate the fundamental properties of more than 500 main-sequence and sub-giant stars. Data obtained during the first 10 months of Kepler science operations were used for this work, when these solar-type targets were observed for one month each in survey mode. Stellar properties have been estimated using two global asteroseismic parameters and complementary photometric and spectroscopic data. Homogeneous sets of effective temperatures, T eff, were available for the entire ensemble from complementary photometry; spectroscopic estimates of T eff and [Fe/H] were available from a homogeneous analysis of ground-based data on a subset of 87 stars. We adopt a grid-based analysis, coupling six pipeline codes to 11 stellar evolutionary grids. Through use of these different grid-pipeline combinations we allow implicitly for the impact on the results of stellar model dependencies from commonly used grids, and differences in adopted pipeline methodologies. By using just two global parameters as the seismic inputs we are able to perform a homogenous analysis of all solar-type stars in the asteroseismic cohort, including many targets for which it would not be possible to provide robust estimates of individual oscillation frequencies (due to a combination of low signal-to-noise ratio and short dataset lengths). The median final quoted uncertainties from consolidation of the grid-based analyses are for the full ensemble (spectroscopic subset) approximately 10.8% (5.4%) in mass, 4.4% (2.2%) in radius, 0.017 dex (0.010 dex) in log g, and 4.3% (2.8%) in mean density. Around 36% (57%) of the stars have final age uncertainties smaller than 1 Gyr. These ages will be useful for ensemble studies, but should be treated carefully on a star-by-star basis. Future analyses using individual oscillation frequencies will offer significant improvements on up to 150 stars, in particular for estimates of the ages, where having the individual frequency data is most important.
dc.publisherInstitute of Physics Publishing
dc.rightsAuthor/s retain copyright
dc.sourceAstrophysical Journal Supplement Series
dc.titleAsteroseismic fundamental properties of solar-type stars observed by the NASA Kepler mission
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume210
dc.date.issued2014
local.identifier.absfor020100 - ASTRONOMICAL AND SPACE SCIENCES
local.identifier.ariespublicationU3488905xPUB1847
local.type.statusPublished Version
local.contributor.affiliationChaplin, W J, University of Birmingham
local.contributor.affiliationBasu, S, Yale University
local.contributor.affiliationHuber, D, NASA Ames Research Center
local.contributor.affiliationSerenelli, Aldo, Instituto de Ciencias del Espacio (CSIC-IEEC)
local.contributor.affiliationCasagrande, Luca, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationSilva Aguirre, V, Aarhus University
local.contributor.affiliationBall, W.H., Max-Planck-Institut fur Sonnensystemforschung
local.contributor.affiliationCreevey, O L, Universite de Nice Sophia Antipolis
local.contributor.affiliationGizon, L, Georg-August-Universitat Gottingen
local.contributor.affiliationHandberg, R., University of Bermingham
local.contributor.affiliationKaroff, C., Aarhus University
local.bibliographicCitation.issue1
local.bibliographicCitation.startpage1
local.bibliographicCitation.lastpage22
local.identifier.doi10.1088/0067-0049/210/1/1
dc.date.updated2015-12-10T11:20:16Z
local.identifier.scopusID2-s2.0-84892742694
local.identifier.thomsonID000328265100001
dcterms.accessRightsOpen Access
CollectionsANU Research Publications

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