A detection of the evolutionary time scale of the da white dwarf G117-B15A with the Whole Earth Telescope
dc.contributor.author | Kepler, Souza Oliveira | pt_BR |
dc.contributor.author | Winget, Donald Earl | pt_BR |
dc.contributor.author | Nather, R. Edward | pt_BR |
dc.contributor.author | Bradley, Paul A. | pt_BR |
dc.contributor.author | Grauer, Albert D. | pt_BR |
dc.contributor.author | Fontaine, Gilles | pt_BR |
dc.contributor.author | Bergeron, Pierre | pt_BR |
dc.contributor.author | Vauclair, Gérard | pt_BR |
dc.contributor.author | Claver, C.F. | pt_BR |
dc.contributor.author | Marar, T.M. Krishnan | pt_BR |
dc.contributor.author | Seetha, S. | pt_BR |
dc.contributor.author | Ashoka, B.N. | pt_BR |
dc.contributor.author | Mazeh, Tsevi | pt_BR |
dc.contributor.author | Leibowitz, Elia M. | pt_BR |
dc.contributor.author | Dolez, Noël | pt_BR |
dc.contributor.author | Chevreton, Michel | pt_BR |
dc.contributor.author | Barstow, Martin A. | pt_BR |
dc.contributor.author | Clemens, J. Christopher | pt_BR |
dc.contributor.author | Kleinman, Scot James | pt_BR |
dc.contributor.author | Sansom, A.E. | pt_BR |
dc.contributor.author | Tweedy, R.W. | pt_BR |
dc.contributor.author | Hine, B.P. | pt_BR |
dc.contributor.author | Provencal, Judith L. | pt_BR |
dc.contributor.author | Wesemael, F. | pt_BR |
dc.contributor.author | Wood, Matthew A. | pt_BR |
dc.contributor.author | Brassard, P. | pt_BR |
dc.contributor.author | Solheim, Jan-Eric | pt_BR |
dc.contributor.author | Emanuelsen, P.-I. | pt_BR |
dc.contributor.author | Kanaan Neto, Antonio Nemer | pt_BR |
dc.contributor.author | Kepler, Souza Oliveira | pt_BR |
dc.date.accessioned | 2014-12-31T02:10:49Z | pt_BR |
dc.date.issued | 1991 | pt_BR |
dc.identifier.issn | 0004-637X | pt_BR |
dc.identifier.uri | http://hdl.handle.net/10183/108717 | pt_BR |
dc.description.abstract | We have detected the time rate of change for the main pulsation period of the 13,000 K DA white dwarf G117-B15A, using the Whole Earth Telescope (WET). The observed rate of period change, P = (12.0 ± 3.5) x 10- 15 s s - ', is somewhat larger than the published theoretical calculations of the rate of period change due to cooling, based on carbon core white dwarf models. We discuss other effects that could contribute to the observed rate of period change. | en |
dc.format.mimetype | application/pdf | |
dc.language.iso | eng | pt_BR |
dc.relation.ispartof | The Astrophysical Journal. Chicago. Vol. 378, no. 2, pt. 2 (Sept. 1991), p. l45-l48 | pt_BR |
dc.rights | Open Access | en |
dc.subject | Stars: evolution | en |
dc.subject | Anãs brancas | pt_BR |
dc.subject | Evolucao estelar | pt_BR |
dc.subject | Stars: variables | en |
dc.subject | Pulsacoes estelares | pt_BR |
dc.subject | Stars: white dwarfs | en |
dc.subject | Estrelas binarias | pt_BR |
dc.subject | Estrelas variaveis | pt_BR |
dc.subject | Fotometria estelar | pt_BR |
dc.subject | Observações astronômicas no visível | pt_BR |
dc.title | A detection of the evolutionary time scale of the da white dwarf G117-B15A with the Whole Earth Telescope | pt_BR |
dc.type | Artigo de periódico | pt_BR |
dc.identifier.nrb | 000055249 | pt_BR |
dc.type.origin | Estrangeiro | pt_BR |
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