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dc.contributor.authorBergeron, Pierrept_BR
dc.contributor.authorFontaine, Gillespt_BR
dc.contributor.authorBrassard, P.pt_BR
dc.contributor.authorLamontagne, R.pt_BR
dc.contributor.authorWesemael, F.pt_BR
dc.contributor.authorWinget, Donald Earlpt_BR
dc.contributor.authorNather, R. Edwardpt_BR
dc.contributor.authorBradley, Paul A.pt_BR
dc.contributor.authorClaver, C.F.pt_BR
dc.contributor.authorClemens, J. Christopherpt_BR
dc.contributor.authorKleinman, Scot Jamespt_BR
dc.contributor.authorProvencal, Judith L.pt_BR
dc.contributor.authorMcgraw, J.T.pt_BR
dc.contributor.authorBirch, P.pt_BR
dc.contributor.authorCandy, M.pt_BR
dc.contributor.authorBuckley, David A.H.pt_BR
dc.contributor.authorTripe, P.pt_BR
dc.contributor.authorAugusteijn, T.pt_BR
dc.contributor.authorVauclair, Gérardpt_BR
dc.contributor.authorKepler, Souza Oliveirapt_BR
dc.contributor.authorKanaan Neto, Antonio Nemerpt_BR
dc.date.accessioned2014-12-04T02:13:39Zpt_BR
dc.date.issued1993pt_BR
dc.identifier.issn0004-6256pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/107731pt_BR
dc.description.abstractNew high-speed photometric observations ofthe pulsating DA white dwarfGD 165 are presented. The Fourier spectrum ofthe light curve ofGD 165 exhibits two main regions ofpower at 120 and 193 s. The presence of a high-amplitude long period mode near ~1800 s reported by Bergeron and McGraw is not confirmed by these new observations. Light curves obtained with the Canada-France-Hawaii Telescope reveal previously undetected low-amplitude harmonic oscillations. Observations with the Whole Earth Telescope are used to resolve the two principal regions of power. The 120 and 193 s peaks are shown to be multiplets composed of at least three, and possibly tive frequency components. The most likely explanation is that these two peaks correspond to nonradial gravity modes with different values of the radial order k and with I= 1 or 2 split into 21+1 components by slow rotation. The frequency differences observed between the three dominant components of each peak are consistent with equal spacing, but a slight asymmetry in spacing cannot be totally ruled out at this stage. They suggest a rotation time scale of the order of 4.2 days. Within a peak, power is not distributed evenly or symmetrically among the three frequency components, particularly for the 193 s mode. Consequently, a simple interpretation in terms of geometric effects (inclination of the pulsation axis with respect to the line of sight) cannot be invoked here. The tentative identification of modes with l=1 or 2 is used to constrain the hydrogen layer mass in GD 165. In particular, the 120 s pulsation mode has a period sufficiently short that useful limits can be derived on this quantity. Using recent adiabatic pulsation calculations and new determinations of the atmospheric parameters of GD 165, it is found that ..(H)/*~>10-3.7 or~>10-6.4 if the 120 s pulsation is a mode with l=1 or 2, respectively.en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofThe Astronomical Journal. New York. Vol. 106, no. 5 (Nov. 1993), p. 1987-1999pt_BR
dc.rightsOpen Accessen
dc.subjectAstrofisica estelarpt_BR
dc.subjectObservacoes astronomicaspt_BR
dc.titleHigh-speed photometric observations of the pulsating da white dwarf gd 165pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000056796pt_BR
dc.type.originEstrangeiropt_BR


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