Asteroseismological measurements on PG 1159-035, the prototype of the GW Virginis variable stars
Autor(a) principal: | |
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Data de Publicação: | 2008 |
Outros Autores: | , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/99027 |
Resumo: | Aims. An asteroseismological study of PG 1159−035, the prototype of the GW Vir variable stars, has been performed on the basis of detailed and full PG1159 evolutionary models presented by Miller Bertolami & Althaus (2006, A&A, 454, 845). Methods. We carried out extensive computations of adiabatic g-mode pulsation periods on PG1159 evolutionary models with stellar masses spanning the range 0.530 to 0.741 Mʘ. These models were derived from the complete evolution of progenitor stars, including the thermally pulsing AGB phase and the born-again episode. We constrained the stellar mass of PG 1159−035 by comparing the observed period spacing with the asymptotic period spacing and with the average of the computed period spacings. We also employed the individual observed periods reported by Costa et al. (2007) to find a representative seismological model for PG 1159−035. Results. We derive a stellar mass in the range 0.56–0.59 M from the period-spacing data alone. We also find, on the basis of a period-fit procedure, an asteroseismological model representative of PG 1159−035 that reproduces the observed period pattern with an average of the period differences of δΠi = 0.64–1.03 s, consistent with the expected model uncertainties. The model has an effective temperature Teff = 128 000+8600 −2600 K, a stellar mass M∗ = 0.565+0.025 −0.009 Mʘ , a surface gravity log g = 7.42+0.21 −0.12, a stellar luminosity and radius of log(L∗/L ) = 2.15 ± 0.08 and log(R∗/R ) = −1.62+0.06 −0.09, and a He-rich envelope thickness of Menv = 0.017 M . The results of the period-fit analysis carried out in this work suggest that the surface gravity of PG 1159−035 would be 1σ larger than the spectroscopically inferred gravity. For our best-fit model of PG 1159−035, all of the pulsation modes are characterized by positive rates of period changes, at odds with the measurements by Costa & Kepler (2007, A&A, submitted). |
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Córsico, Alejandro HugoAlthaus, Leandro GabrielKepler, Souza OliveiraCosta, Jose Eduardo da SilveiraMiller Bertolami, Marcelo Miguel2014-08-01T02:07:09Z20080004-6361http://hdl.handle.net/10183/99027000625008Aims. An asteroseismological study of PG 1159−035, the prototype of the GW Vir variable stars, has been performed on the basis of detailed and full PG1159 evolutionary models presented by Miller Bertolami & Althaus (2006, A&A, 454, 845). Methods. We carried out extensive computations of adiabatic g-mode pulsation periods on PG1159 evolutionary models with stellar masses spanning the range 0.530 to 0.741 Mʘ. These models were derived from the complete evolution of progenitor stars, including the thermally pulsing AGB phase and the born-again episode. We constrained the stellar mass of PG 1159−035 by comparing the observed period spacing with the asymptotic period spacing and with the average of the computed period spacings. We also employed the individual observed periods reported by Costa et al. (2007) to find a representative seismological model for PG 1159−035. Results. We derive a stellar mass in the range 0.56–0.59 M from the period-spacing data alone. We also find, on the basis of a period-fit procedure, an asteroseismological model representative of PG 1159−035 that reproduces the observed period pattern with an average of the period differences of δΠi = 0.64–1.03 s, consistent with the expected model uncertainties. The model has an effective temperature Teff = 128 000+8600 −2600 K, a stellar mass M∗ = 0.565+0.025 −0.009 Mʘ , a surface gravity log g = 7.42+0.21 −0.12, a stellar luminosity and radius of log(L∗/L ) = 2.15 ± 0.08 and log(R∗/R ) = −1.62+0.06 −0.09, and a He-rich envelope thickness of Menv = 0.017 M . The results of the period-fit analysis carried out in this work suggest that the surface gravity of PG 1159−035 would be 1σ larger than the spectroscopically inferred gravity. For our best-fit model of PG 1159−035, all of the pulsation modes are characterized by positive rates of period changes, at odds with the measurements by Costa & Kepler (2007, A&A, submitted).application/pdfengAstronomy and Astrophysics. Berlin. Vol. 478, no. 3 (Feb. 2008), p. 869-881AsterosismologiaAnãs brancasEvolucao estelarAstrofísicaStars: evolutionStars: interiorsStars: oscillationsStars: variables: generalStars: white dwarfsStars: individual: PG 1159-035Asteroseismological measurements on PG 1159-035, the prototype of the GW Virginis variable starsEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSORIGINAL000625008.pdf000625008.pdfTexto completo (inglês)application/pdf670364http://www.lume.ufrgs.br/bitstream/10183/99027/1/000625008.pdf65ce68bcc3f48f458ddc732c7bc13e82MD51TEXT000625008.pdf.txt000625008.pdf.txtExtracted Texttext/plain75000http://www.lume.ufrgs.br/bitstream/10183/99027/2/000625008.pdf.txt405d3d42b0aff5c6129523d1048a1b23MD52THUMBNAIL000625008.pdf.jpg000625008.pdf.jpgGenerated Thumbnailimage/jpeg2157http://www.lume.ufrgs.br/bitstream/10183/99027/3/000625008.pdf.jpgc5d1cd446a86620c459f4b4fe6ff7289MD5310183/990272023-08-16 03:32:00.759194oai:www.lume.ufrgs.br:10183/99027Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-08-16T06:32Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Asteroseismological measurements on PG 1159-035, the prototype of the GW Virginis variable stars |
title |
Asteroseismological measurements on PG 1159-035, the prototype of the GW Virginis variable stars |
spellingShingle |
Asteroseismological measurements on PG 1159-035, the prototype of the GW Virginis variable stars Córsico, Alejandro Hugo Asterosismologia Anãs brancas Evolucao estelar Astrofísica Stars: evolution Stars: interiors Stars: oscillations Stars: variables: general Stars: white dwarfs Stars: individual: PG 1159-035 |
title_short |
Asteroseismological measurements on PG 1159-035, the prototype of the GW Virginis variable stars |
title_full |
Asteroseismological measurements on PG 1159-035, the prototype of the GW Virginis variable stars |
title_fullStr |
Asteroseismological measurements on PG 1159-035, the prototype of the GW Virginis variable stars |
title_full_unstemmed |
Asteroseismological measurements on PG 1159-035, the prototype of the GW Virginis variable stars |
title_sort |
Asteroseismological measurements on PG 1159-035, the prototype of the GW Virginis variable stars |
author |
Córsico, Alejandro Hugo |
author_facet |
Córsico, Alejandro Hugo Althaus, Leandro Gabriel Kepler, Souza Oliveira Costa, Jose Eduardo da Silveira Miller Bertolami, Marcelo Miguel |
author_role |
author |
author2 |
Althaus, Leandro Gabriel Kepler, Souza Oliveira Costa, Jose Eduardo da Silveira Miller Bertolami, Marcelo Miguel |
author2_role |
author author author author |
dc.contributor.author.fl_str_mv |
Córsico, Alejandro Hugo Althaus, Leandro Gabriel Kepler, Souza Oliveira Costa, Jose Eduardo da Silveira Miller Bertolami, Marcelo Miguel |
dc.subject.por.fl_str_mv |
Asterosismologia Anãs brancas Evolucao estelar Astrofísica |
topic |
Asterosismologia Anãs brancas Evolucao estelar Astrofísica Stars: evolution Stars: interiors Stars: oscillations Stars: variables: general Stars: white dwarfs Stars: individual: PG 1159-035 |
dc.subject.eng.fl_str_mv |
Stars: evolution Stars: interiors Stars: oscillations Stars: variables: general Stars: white dwarfs Stars: individual: PG 1159-035 |
description |
Aims. An asteroseismological study of PG 1159−035, the prototype of the GW Vir variable stars, has been performed on the basis of detailed and full PG1159 evolutionary models presented by Miller Bertolami & Althaus (2006, A&A, 454, 845). Methods. We carried out extensive computations of adiabatic g-mode pulsation periods on PG1159 evolutionary models with stellar masses spanning the range 0.530 to 0.741 Mʘ. These models were derived from the complete evolution of progenitor stars, including the thermally pulsing AGB phase and the born-again episode. We constrained the stellar mass of PG 1159−035 by comparing the observed period spacing with the asymptotic period spacing and with the average of the computed period spacings. We also employed the individual observed periods reported by Costa et al. (2007) to find a representative seismological model for PG 1159−035. Results. We derive a stellar mass in the range 0.56–0.59 M from the period-spacing data alone. We also find, on the basis of a period-fit procedure, an asteroseismological model representative of PG 1159−035 that reproduces the observed period pattern with an average of the period differences of δΠi = 0.64–1.03 s, consistent with the expected model uncertainties. The model has an effective temperature Teff = 128 000+8600 −2600 K, a stellar mass M∗ = 0.565+0.025 −0.009 Mʘ , a surface gravity log g = 7.42+0.21 −0.12, a stellar luminosity and radius of log(L∗/L ) = 2.15 ± 0.08 and log(R∗/R ) = −1.62+0.06 −0.09, and a He-rich envelope thickness of Menv = 0.017 M . The results of the period-fit analysis carried out in this work suggest that the surface gravity of PG 1159−035 would be 1σ larger than the spectroscopically inferred gravity. For our best-fit model of PG 1159−035, all of the pulsation modes are characterized by positive rates of period changes, at odds with the measurements by Costa & Kepler (2007, A&A, submitted). |
publishDate |
2008 |
dc.date.issued.fl_str_mv |
2008 |
dc.date.accessioned.fl_str_mv |
2014-08-01T02:07:09Z |
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Estrangeiro info:eu-repo/semantics/article |
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0004-6361 |
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000625008 |
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http://hdl.handle.net/10183/99027 |
dc.language.iso.fl_str_mv |
eng |
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dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy and Astrophysics. Berlin. Vol. 478, no. 3 (Feb. 2008), p. 869-881 |
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