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dc.contributor.authorVuckovic, Majapt_BR
dc.contributor.authorKawaler, Steven D.pt_BR
dc.contributor.authorO'Toole, Simonpt_BR
dc.contributor.authorCsubry, Z.pt_BR
dc.contributor.authorBaran, Andrzejpt_BR
dc.contributor.authorZola, Staszekpt_BR
dc.contributor.authorMoskalik, Pawelpt_BR
dc.contributor.authorKlumpe, Eric W.pt_BR
dc.contributor.authorRiddle, Reed L.pt_BR
dc.contributor.authorO'Brien, M. Seanpt_BR
dc.contributor.authorMullally, Fergalpt_BR
dc.contributor.authorWood, Matthew A.pt_BR
dc.contributor.authorWilkat, Vanessapt_BR
dc.contributor.authorZhou, Ai-Yingpt_BR
dc.contributor.authorReed, M. D.pt_BR
dc.contributor.authorTerndrup, Donald M.pt_BR
dc.contributor.authorSullivan, Denis J.pt_BR
dc.contributor.authorKim, Seung-Leept_BR
dc.contributor.authorChen, Wen-Pingpt_BR
dc.contributor.authorChen, C.-W.pt_BR
dc.contributor.authorHsiao, Wen-Shanpt_BR
dc.contributor.authorKausharbanu, Sanchawalapt_BR
dc.contributor.authorLee, Hsu-Taipt_BR
dc.contributor.authorJiang, Xiaojunpt_BR
dc.contributor.authorJanulis, Rimvydaspt_BR
dc.contributor.authorSiwak, Michalpt_BR
dc.contributor.authorOgloza, Waldemarpt_BR
dc.contributor.authorPaparo, Margitpt_BR
dc.contributor.authorBognár, Zsófiapt_BR
dc.contributor.authorSódor, Ádámpt_BR
dc.contributor.authorHandler, Geraldpt_BR
dc.contributor.authorLorenz, Denisept_BR
dc.contributor.authorSteininger, Brunopt_BR
dc.contributor.authorSilvotti, Robertopt_BR
dc.contributor.authorVauclair, Gérardpt_BR
dc.contributor.authorOreiro, Raquelpt_BR
dc.contributor.authorOstensen, Roypt_BR
dc.contributor.authorBronowska, A.pt_BR
dc.contributor.authorCastanheira, Bárbara Garciapt_BR
dc.contributor.authorKepler, Souza Oliveirapt_BR
dc.contributor.authorFraga, Lucianopt_BR
dc.contributor.authorShipman, Harry L.pt_BR
dc.contributor.authorProvencal, Judith L.pt_BR
dc.contributor.authorChilders, D.pt_BR
dc.date.accessioned2015-01-14T02:15:58Zpt_BR
dc.date.issued2006pt_BR
dc.identifier.issn0004-637Xpt_BR
dc.identifier.urihttp://hdl.handle.net/10183/108919pt_BR
dc.description.abstractPG 0014+067 is one of the most promising pulsating subdwarf B stars for seismic analysis, as it has a rich pulsation spectrum. The richness of its pulsations, however, poses a fundamental challenge to understanding the pulsations of these stars, as the mode density is too complex to be explained only with radial and nonradial low-degree (l< 3) p-modes without rotational splittings. One proposed solution, suggested by Brassard et al. in 2001 for the case of PG 0014+067 in particular, assigns some modes with high degree (l=3). On the other hand, theoretical models of sdB stars suggest that they may retain rapidly rotating cores, and so the high mode density may result from the presence of a few rotationally split triplet (l = 1) and quintuplet (l = 2) modes, along with radial (l = 0) p-modes. To examine alternative theoretical models for these stars, we need better frequency resolution and denser longitude coverage. Therefore, we observed this star with the Whole Earth Telescope for two weeks in 2004 October. In this paper we report the results of Whole Earth Telescope observations of the pulsating subdwarf B star PG 0014+067.We find that the frequencies seen in PG 0014+067 do not appear to fit any theoretical model currently available; however, we find a simple empirical relation that is able to match all of the well-determined frequencies in this star.en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofThe astrophysical journal. Chicago. Vol. 646, no. 2, pt. 1 (Aug. 2006), p. 1230-1240pt_BR
dc.rightsOpen Accessen
dc.subjectStars: individual (PG 0014+067)en
dc.subjectPulsacoes estelarespt_BR
dc.subjectAnãs brancaspt_BR
dc.subjectStars: oscillationsen
dc.subjectObservacoes astronomicaspt_BR
dc.subjectSubdwarfsen
dc.subjectTelescopiospt_BR
dc.titleWhole Earth Telescope observations of the pulsating subdwarf B star PG 0014+067pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000558602pt_BR
dc.type.originEstrangeiropt_BR


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