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Whole Earth Telescope observations of the DAV white dwarf G226-29

dc.contributor.authorKepler, Souza Oliveirapt_BR
dc.contributor.authorGiovannini Junior, Odilonpt_BR
dc.contributor.authorWood, Matthew A.pt_BR
dc.contributor.authorNather, R. Edwardpt_BR
dc.contributor.authorWinget, Donald Earlpt_BR
dc.contributor.authorKanaan Neto, Antonio Nemerpt_BR
dc.contributor.authorKleinman, Scot Jamespt_BR
dc.contributor.authorBradley, Paul A.pt_BR
dc.contributor.authorProvencal, Judith L.pt_BR
dc.contributor.authorClemens, J. Christopherpt_BR
dc.contributor.authorClaver, C.F.pt_BR
dc.contributor.authorWatson, Todd K.pt_BR
dc.contributor.authorYanagida, K.pt_BR
dc.contributor.authorKrisciunas, K.pt_BR
dc.contributor.authorMarar, T.M. Krishnanpt_BR
dc.contributor.authorSeetha, S.pt_BR
dc.contributor.authorAshoka, B.N.pt_BR
dc.contributor.authorLeibowitz, Elia M.pt_BR
dc.contributor.authorMendelson, Haimpt_BR
dc.contributor.authorMazeh, Tsevipt_BR
dc.contributor.authorMoskalik, Pawelpt_BR
dc.contributor.authorKrzesinski, Jerzypt_BR
dc.contributor.authorPajdosz, Y.pt_BR
dc.contributor.authorZola, Staszekpt_BR
dc.contributor.authorSolheim, Jan-Ericpt_BR
dc.contributor.authorEmanuelsen, P.-I.pt_BR
dc.contributor.authorDolez, Noëlpt_BR
dc.contributor.authorVauclair, Gérardpt_BR
dc.contributor.authorChevreton, Michelpt_BR
dc.contributor.authorFremy, J. R.pt_BR
dc.contributor.authorBarstow, Martin A.pt_BR
dc.contributor.authorSansom, A.E.pt_BR
dc.contributor.authorTweedy, R.W.pt_BR
dc.contributor.authorWickramasinghe, D.T.pt_BR
dc.contributor.authorFerrario, Liliapt_BR
dc.contributor.authorSullivan, Denis J.pt_BR
dc.contributor.authorPeet, A.J. van derpt_BR
dc.contributor.authorBuckley, David A.H.pt_BR
dc.contributor.authorChen, A.-L.pt_BR
dc.date.accessioned2015-01-13T02:14:48Zpt_BR
dc.date.issued1995pt_BR
dc.identifier.issn0004-637Xpt_BR
dc.identifier.urihttp://hdl.handle.net/10183/108901pt_BR
dc.description.abstractWe observed G226-29 for 121 hr in 1992 February and confirm the presence of the three previously identified frequencies close to 109 s. We find no evidence of other pulsation periods down to our noise level of about 0.35 millimodulation amplitudes. The presence of only one triplet pulsation mode in G226-29 and its effective temperature near the blue edge of the instability strip identify the observed triplet of modes near 109 s as rotationally split components of the k = 1, l = 1 mode. With the mode identification, we derived a rotation period of 8.9 hr and an inclination of the pulsation axis of 70°-75° to our line of sight.en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofThe astrophysical Journal. Chicago. Vol. 447, no. 2, pt. 1 (July 1995), p. 874-879pt_BR
dc.rightsOpen Accessen
dc.subjectAstrofisica estelarpt_BR
dc.subjectStars: individual (G226-29)en
dc.subjectEstrelas variaveispt_BR
dc.subjectStars: oscillationsen
dc.subjectPulsacoes estelarespt_BR
dc.subjectStars: rotationen
dc.subjectWhite dwarfsen
dc.subjectAnãs brancaspt_BR
dc.titleWhole Earth Telescope observations of the DAV white dwarf G226-29pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000262832pt_BR
dc.type.originEstrangeiropt_BR


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