Mostrar registro simples

dc.contributor.authorKawaler, Steven D.pt_BR
dc.contributor.authorPotter, E. M.pt_BR
dc.contributor.authorVuckovic, Majapt_BR
dc.contributor.authorO'Toole, Simonpt_BR
dc.contributor.authorClemens, J. Christopherpt_BR
dc.contributor.authorO'Brien, M. Seanpt_BR
dc.contributor.authorGrauer, Albert D.pt_BR
dc.contributor.authorNather, R. Edwardpt_BR
dc.contributor.authorMoskalik, Pawelpt_BR
dc.contributor.authorFontaine, Gillespt_BR
dc.contributor.authorWesemael, F.pt_BR
dc.contributor.authorBergeron, Pierrept_BR
dc.contributor.authorVauclair, Gérardpt_BR
dc.contributor.authorDolez, Noëlpt_BR
dc.contributor.authorChevreton, Michelpt_BR
dc.contributor.authorKleinman, Scot Jamespt_BR
dc.contributor.authorWatson, Todd K.pt_BR
dc.contributor.authorBarstow, Martin A.pt_BR
dc.contributor.authorDind, Z. E.pt_BR
dc.contributor.authorSansom, A.E.pt_BR
dc.contributor.authorWinget, Donald Earlpt_BR
dc.contributor.authorKepler, Souza Oliveirapt_BR
dc.contributor.authorKanaan Neto, Antonio Nemerpt_BR
dc.contributor.authorBradley, Paul A.pt_BR
dc.contributor.authorDixson, James S.pt_BR
dc.contributor.authorProvencal, Judith L.pt_BR
dc.contributor.authorBedding, T. R.pt_BR
dc.date.accessioned2014-07-26T02:09:17Zpt_BR
dc.date.issued2004pt_BR
dc.identifier.issn0004-6361pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/98766pt_BR
dc.description.abstractWe report on the analysis of multisite time-series photometry of the pulsating pre-white dwarf (GW Vir star) PG 1707+427, obtained by the Whole Earth Telescope collaboration. This is the last of the known GW Vir stars without surrounding nebulae to be resolved by multisite data. Successful resolution of the pulsation spectrum resulted from the combination of high signal-to-noise observations with a large telescope and wide coverage in longitude with smaller telescopes. We find a series of 8 pulsation frequencies (along with two nonlinear combination frequencies), and identify 7 of them as part of a sequence of l = 1 modes, with a common period spacing of 23.0 s. This spacing implies that the mass of PG 1707+427 is 0.57 Mѳ. Preliminary model fits suggest that the mass determined via asteroseismology is consistent with the mass determined from spectroscopy combined with evolutionary tracks.en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofAstronomy and Astrophysics. Berlin. Vol. 428, no. 3 (Dec. 2004), p. 969-981pt_BR
dc.rightsOpen Accessen
dc.subjectStars: evolutionen
dc.subjectAstrofisica estelarpt_BR
dc.subjectEvolucao estelarpt_BR
dc.subjectStars: white dwarfsen
dc.subjectFotometria estelarpt_BR
dc.subjectStars: oscillationsen
dc.subjectPulsacoes estelarespt_BR
dc.subjectStars: individual: PG 1707+427en
dc.subjectEspectros estelarespt_BR
dc.subjectAnãs brancaspt_BR
dc.titleWhole earth telescope observations of the pulsating hot white dwarf PG 1707+427pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000504047pt_BR
dc.type.originEstrangeiropt_BR


Thumbnail
   

Este item está licenciado na Creative Commons License

Mostrar registro simples