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Determining distances using asteroseismic methods

Silva Aguirre, V; Casagrande, Luca; Basu, S; Campante, T. L.; Chaplin, W J; Huber, D; Miglio, A; Serenelli, Aldo

Description

Asteroseismology has been extremely successful in determining the properties of stars in different evolutionary stages with a remarkable level of precision. However, to fully exploit its potential, robust methods for estimating stellar parameters are required and independent verification of the results is needed. In this talk, I present a new technique developed to obtain stellar properties by coupling asteroseismic analysis with the infrared flux method. Using two global seismic observables...[Show more]

dc.contributor.authorSilva Aguirre, V
dc.contributor.authorCasagrande, Luca
dc.contributor.authorBasu, S
dc.contributor.authorCampante, T. L.
dc.contributor.authorChaplin, W J
dc.contributor.authorHuber, D
dc.contributor.authorMiglio, A
dc.contributor.authorSerenelli, Aldo
dc.date.accessioned2015-12-13T22:16:21Z
dc.identifier.issn0004-6337
dc.identifier.urihttp://hdl.handle.net/1885/70820
dc.description.abstractAsteroseismology has been extremely successful in determining the properties of stars in different evolutionary stages with a remarkable level of precision. However, to fully exploit its potential, robust methods for estimating stellar parameters are required and independent verification of the results is needed. In this talk, I present a new technique developed to obtain stellar properties by coupling asteroseismic analysis with the infrared flux method. Using two global seismic observables and multi-band photometry, the technique determines masses, radii, effective temperatures, bolometric fluxes, and thus distances for field stars in a self-consistent manner. Applying our method to a sample of solar-like oscillators in the Kepler field that have accurate Hipparcos parallaxes, we find agreement in our distance determinations to better than 5 %. Comparison with measurements of spectroscopic effective temperatures and interferometric radii also validate our results, and show that our technique can be applied to stars evolved beyond the main-sequence phase.
dc.publisherWiley-VCH Verlag GMBH
dc.sourceAstronomische Nachrichten
dc.subjectKeywords: Stars: distances; Stars: fundamental parameters; Stars: oscillations; Techniques: photometric
dc.titleDetermining distances using asteroseismic methods
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume334
dc.date.issued2013
local.identifier.absfor020102 - Astronomical and Space Instrumentation
local.identifier.ariespublicationf5625xPUB2429
local.type.statusPublished Version
local.contributor.affiliationSilva Aguirre, V, Aarhus University
local.contributor.affiliationCasagrande, Luca, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationBasu, S, Yale University
local.contributor.affiliationCampante, T. L., Universidade do Porto
local.contributor.affiliationChaplin, W J, University of Birmingham
local.contributor.affiliationHuber, D, NASA Ames Research Center
local.contributor.affiliationMiglio, A, University of Birmingham
local.contributor.affiliationSerenelli, Aldo, Instituto de Ciencias del Espacio (CSIC-IEEC)
local.description.embargo2037-12-31
local.bibliographicCitation.issue1-2
local.bibliographicCitation.startpage22
local.bibliographicCitation.lastpage25
local.identifier.doi10.1002/asna.201211774
dc.date.updated2016-02-24T08:58:24Z
local.identifier.scopusID2-s2.0-84873468474
local.identifier.thomsonID000325859900006
CollectionsANU Research Publications

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