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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/5005
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dc.contributor.authorChaplin, W. J-
dc.contributor.authorAppourchaux, T-
dc.contributor.authorElsworth, Y-
dc.contributor.authorGarcia, R. A-
dc.contributor.authorHoudek, G-
dc.contributor.authorKaroff, C-
dc.contributor.authorMetcalfe, T. S-
dc.contributor.authorMolenda-Zakowicz, J-
dc.contributor.authorMonteiro, M. J. P. F. G-
dc.contributor.authorThompson, M. J-
dc.contributor.authorBrown, T. M-
dc.contributor.authorKiss, L. L-
dc.contributor.authorKitiashvili, I. N-
dc.contributor.authorKolenberg, K-
dc.contributor.authorKorhonen, H-
dc.contributor.authorKosovichev, A. G-
dc.contributor.authorKupka, F-
dc.contributor.authorLebreton, Y-
dc.contributor.authorLeroy, B-
dc.contributor.authorLudwig, H. G-
dc.contributor.authorMathis, S-
dc.contributor.authorMichel, E-
dc.contributor.authorMiglio, A-
dc.contributor.authorMontalban, J-
dc.contributor.authorMoya, A-
dc.contributor.authorNoels, A-
dc.contributor.authorNoyes, R. W-
dc.contributor.authorPalle, P. L-
dc.contributor.authorPiau, L-
dc.contributor.authorPreston, H. L-
dc.contributor.authorRoca Cortes, T-
dc.contributor.authorRoth, M-
dc.contributor.authorSato, K. H-
dc.contributor.authorSchmitt, J-
dc.contributor.authorSerenelli, A. M-
dc.contributor.authorSilva Aguirre, V-
dc.contributor.authorStevens, I. R-
dc.contributor.authorSuarez, J. C-
dc.contributor.authorSuran, M. D-
dc.contributor.authorTrampedach, R-
dc.contributor.authorTurck-Chieze, S-
dc.contributor.authorUytterhoeven, K-
dc.contributor.authorVentura, R-
dc.contributor.authorChristensen-Dalsgaard, J-
dc.contributor.authorGilliland, R. L-
dc.contributor.authorKjeldsen, H-
dc.contributor.authorBorucki, W. J-
dc.contributor.authorKoch, D-
dc.contributor.authorJenkins, J. M-
dc.contributor.authorBallot, J-
dc.contributor.authorBasu, S-
dc.contributor.authorBazot, M-
dc.contributor.authorBedding, T. R-
dc.contributor.authorBenomar, O-
dc.contributor.authorBonanno, A-
dc.contributor.authorBrandao, I. M-
dc.contributor.authorBruntt, H-
dc.contributor.authorCampante, T. L-
dc.contributor.authorCreevey, O. L-
dc.contributor.authorDi Mauro, M. P-
dc.contributor.authorDogan, G-
dc.contributor.authorDreizler, S-
dc.contributor.authorEggenberger, P-
dc.contributor.authorEsch, L-
dc.contributor.authorFletcher, S. T-
dc.contributor.authorFrandsen, S-
dc.contributor.authorGai, N-
dc.contributor.authorGaulme, P-
dc.contributor.authorHandberg, R-
dc.contributor.authorHekker, S-
dc.contributor.authorHowe, R-
dc.contributor.authorHuber, D-
dc.contributor.authorKorzennik, S. G-
dc.contributor.authorLebrun, J. C-
dc.contributor.authorLeccia, S-
dc.contributor.authorMartic, M-
dc.contributor.authorMathur, S-
dc.contributor.authorMosser, B-
dc.contributor.authorNew, R-
dc.contributor.authorQuirion, P. O-
dc.contributor.authorRegulo, C-
dc.contributor.authorRoxburgh, I. W-
dc.contributor.authorSalabert, D-
dc.contributor.authorSchou, J-
dc.contributor.authorSousa, S. G-
dc.contributor.authorStello, D-
dc.contributor.authorVerner, G. A-
dc.contributor.authorArentoft, T-
dc.contributor.authorBarban, C-
dc.contributor.authorBelkacem, K-
dc.contributor.authorBenatti, S-
dc.contributor.authorBiazzo, K-
dc.contributor.authorBoumier, P-
dc.contributor.authorBradley, P. A-
dc.contributor.authorBroomhall, A. M-
dc.contributor.authorBuzasi, D. L-
dc.contributor.authorClaudi, R. U-
dc.contributor.authorCunha, M. S-
dc.contributor.authorD'Antona, F-
dc.contributor.authorDeheuvels, S-
dc.contributor.authorDerekas, A-
dc.contributor.authorGarcia Hernandez, A-
dc.contributor.authorGiampapa, M. S-
dc.contributor.authorGoupil, M. J-
dc.contributor.authorGruberbauer, M-
dc.contributor.authorGuzik, J. A-
dc.contributor.authorHale, S. J-
dc.contributor.authorIreland, M. J-
dc.date.accessioned2010-02-09T13:38:15Z-
dc.date.available2010-02-09T13:38:15Z-
dc.date.issued2010-04-
dc.identifier.citationThe Astrophysical Journal, Vol. 713, No. 2, pp. L169 - L175en
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/2248/5005-
dc.description.abstractWe present preliminary asteroseismic results from Kepler on three G-type stars. The observations, made at one-minute cadence during the first 33.5d of science operations, reveal high signal-to-noise solar-like oscillation spectra in all three stars: About 20 modes of oscillation may be clearly distinguished in each star. We discuss the appearance of the oscillation spectra, use the frequencies and frequency separations to provide first results on the radii, masses and ages of the stars, and comment in the light of these results on prospects for inference on other solar-type stars that Kepler will observe.en
dc.language.isoenen
dc.publisherIOP Publishingen
dc.relation.urihttp://arxiv.org/abs/1001.0506en
dc.relation.urihttp://iopscience.iop.org/2041-8205/713/2/L169/-
dc.rights© Institute of Physicsen
dc.subjectStars: Oscillationsen
dc.subjectStars: Interiorsen
dc.subjectStars: Late-Typeen
dc.titleThe asteroseismic potential of Kepler: first results for solar-type starsen
dc.typeArticleen
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