{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2023,9,1]],"date-time":"2023-09-01T09:15:42Z","timestamp":1693559742893},"reference-count":29,"publisher":"Wiley","issue":"1-2","license":[{"start":{"date-parts":[[2013,2,6]],"date-time":"2013-02-06T00:00:00Z","timestamp":1360108800000},"content-version":"vor","delay-in-days":5,"URL":"http:\/\/onlinelibrary.wiley.com\/termsAndConditions#vor"}],"content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Astron Nachr"],"published-print":{"date-parts":[[2013,2]]},"abstract":"<jats:title>Abstract<\/jats:title><jats:p>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 and multi\u2010band photometry, the technique determines masses, radii, effective temperatures, bolometric fluxes, and thus distances for field stars in a self\u2010consistent manner. Applying our method to a sample of solar\u2010like oscillators in the <jats:italic>Kepler<\/jats:italic> 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\u2010sequence phase. (\u00a9 2013 WILEY\u2010VCH Verlag GmbH &amp; Co. KGaA, Weinheim)<\/jats:p>","DOI":"10.1002\/asna.201211774","type":"journal-article","created":{"date-parts":[[2014,10,15]],"date-time":"2014-10-15T15:30:23Z","timestamp":1413387023000},"page":"22-25","source":"Crossref","is-referenced-by-count":1,"title":["Determining distances using asteroseismic methods"],"prefix":"10.1002","volume":"334","author":[{"given":"V.","family":"Silva Aguirre","sequence":"first","affiliation":[]},{"given":"L.","family":"Casagrande","sequence":"additional","affiliation":[]},{"given":"S.","family":"Basu","sequence":"additional","affiliation":[]},{"given":"T. L.","family":"Campante","sequence":"additional","affiliation":[]},{"given":"W. J.","family":"Chaplin","sequence":"additional","affiliation":[]},{"given":"D.","family":"Huber","sequence":"additional","affiliation":[]},{"given":"A.","family":"Miglio","sequence":"additional","affiliation":[]},{"given":"A. M.","family":"Serenelli","sequence":"additional","affiliation":[]},{"family":"KASC WG#1","sequence":"additional","affiliation":[]}],"member":"311","published-online":{"date-parts":[[2013,2,6]]},"reference":[{"key":"e_1_2_1_2_1","unstructured":"Baglin A. Auvergne M. Barge P. et al.2006 Scientific Objectives for a Minisat: CoRoT in The CoRoT Mission Pre\u2010Launch Status \u2013 Stellar Seismology and Planet Finding ed. M. Fridlund A. Baglin J. Lochard & L. 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