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Observations of the pulsating white dwarf G 185-32

dc.contributor.authorCastanheira, Bárbara Garciapt_BR
dc.contributor.authorKepler, Souza Oliveirapt_BR
dc.contributor.authorMoskalik, Pawelpt_BR
dc.contributor.authorZola, Staszekpt_BR
dc.contributor.authorPajdosz, Gabrielpt_BR
dc.contributor.authorKrzesinski, Jerzypt_BR
dc.contributor.authorO'Donoghue, Darraghpt_BR
dc.contributor.authorKatz, M.pt_BR
dc.contributor.authorBuckley, David A.H.pt_BR
dc.contributor.authorVauclair, Gérardpt_BR
dc.contributor.authorDolez, Noëlpt_BR
dc.contributor.authorChevreton, Michelpt_BR
dc.contributor.authorBarstow, Martin A.pt_BR
dc.contributor.authorKanaan Neto, Antonio Nemerpt_BR
dc.contributor.authorGiovannini Junior, Odilonpt_BR
dc.contributor.authorProvencal, Judith L.pt_BR
dc.contributor.authorKawaler, Steven D.pt_BR
dc.contributor.authorClemens, J. Christopherpt_BR
dc.contributor.authorNather, R. Edwardpt_BR
dc.contributor.authorWinget, Donald Earlpt_BR
dc.contributor.authorWatson, Todd K.pt_BR
dc.contributor.authorYanagida, K.pt_BR
dc.contributor.authorDixson, James S.pt_BR
dc.contributor.authorHansen, Carl J.pt_BR
dc.contributor.authorBradley, Paul A.pt_BR
dc.contributor.authorWood, Matthew A.pt_BR
dc.contributor.authorSullivan, Denis J.pt_BR
dc.contributor.authorKleinman, Scot Jamespt_BR
dc.contributor.authorMeistas, Edmundas G.pt_BR
dc.contributor.authorSolheim, Jan-Ericpt_BR
dc.contributor.authorBruvold, A.pt_BR
dc.contributor.authorLeibowitz, Elia M.pt_BR
dc.contributor.authorMazeh, Tsevipt_BR
dc.contributor.authorKoester, D.pt_BR
dc.contributor.authorMontgomery, Michael Houstonpt_BR
dc.date.accessioned2014-07-24T02:04:25Zpt_BR
dc.date.issued2004pt_BR
dc.identifier.issn0004-6361pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/98518pt_BR
dc.description.abstractWe observed the pulsating hydrogen atmosphere white dwarf G 185–32 with the Whole Earth Telescope in 1992. We report on a weighted Fourier transform of the data detecting 18 periodicities in its light curve. Using the Hubble Space Telescope Faint Object Spectrograph time resolved spectroscopy, and the wavelength dependence of the relative amplitudes, we identify the spherical harmonic degree ( ) for 14 pulsation signals.We also compare the determinations of effective temperature and surface gravity using the excited modes and atmospheric methods, obtaining Teff = 11 960 ± 80 K, log g = 8.02 ± 0.04 and M = 0.617 ± 0.024 M .en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofAstronomy and astrophysics. Vol. 413, no. 2 (Jan. 2004), p. 623-634pt_BR
dc.rightsOpen Accessen
dc.subjectAtmosferas estelarespt_BR
dc.subjectStars: white dwarfsen
dc.subjectStars: variables: generalen
dc.subjectEvolucao estelarpt_BR
dc.subjectFotometria estelarpt_BR
dc.subjectStars: oscillationsen
dc.subjectStars: individual: G 185–32en
dc.subjectPulsacoes estelarespt_BR
dc.subjectStars: evolutionen
dc.subjectAnãs brancaspt_BR
dc.subjectTransformada de Fourierpt_BR
dc.titleObservations of the pulsating white dwarf G 185-32pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000400861pt_BR
dc.type.originEstrangeiropt_BR


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