Asteroseismology of ZZ Ceti stars with fully evolutionary white dwarf models : I. the impact of the uncertainties from prior evolution on the period spectrum
Main Author: | |
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Publication Date: | 2017 |
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Format: | Article |
Language: | eng |
Source: | Repositório Institucional da UFRGS |
Download full: | http://hdl.handle.net/10183/175042 |
Summary: | Context. ZZ Ceti stars are pulsating white dwarfs with a carbon-oxygen core build up during the core helium burning and thermally pulsing Asymptotic Giant Branch phases. Through the interpretation of their pulsation periods by means of asteroseismology, details about their origin and evolution can be inferred. The whole pulsation spectrum exhibited by ZZ Ceti stars strongly depends on the inner chemical structure. At present, there are several processes a ecting the chemical profiles that are still not accurately determined. Aims. We present a study of the impact of the current uncertainties of the white dwarf formation and evolution on the expected pulsation properties of ZZ Ceti stars. Methods. Our analysis is based on a set of carbon-oxygen core white dwarf models with masses 0:548 and 0:837 M that are derived from full evolutionary computations from the ZAMS to the ZZ Ceti domain. We considered models in which we varied the number of thermal pulses, the amount of overshooting, and the 12C( ; )16O reaction rate within their uncertainties. Results. We explore the impact of these major uncertainties in prior evolution on the chemical structure and expected pulsation spectrum. We find that these uncertainties yield significant changes in the g-mode pulsation periods. Conclusions. We conclude that the uncertainties in the white dwarf progenitor evolution should be taken into account in detailed asteroseismological analyses of these pulsating stars. |
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De Gerónimo, Francisco CesarAlthaus, Leandro GabrielCórsico, Alejandro HugoRomero, Alejandra DanielaKepler, Souza Oliveira2018-04-26T02:33:00Z20170004-6361http://hdl.handle.net/10183/175042001063756Context. ZZ Ceti stars are pulsating white dwarfs with a carbon-oxygen core build up during the core helium burning and thermally pulsing Asymptotic Giant Branch phases. Through the interpretation of their pulsation periods by means of asteroseismology, details about their origin and evolution can be inferred. The whole pulsation spectrum exhibited by ZZ Ceti stars strongly depends on the inner chemical structure. At present, there are several processes a ecting the chemical profiles that are still not accurately determined. Aims. We present a study of the impact of the current uncertainties of the white dwarf formation and evolution on the expected pulsation properties of ZZ Ceti stars. Methods. Our analysis is based on a set of carbon-oxygen core white dwarf models with masses 0:548 and 0:837 M that are derived from full evolutionary computations from the ZAMS to the ZZ Ceti domain. We considered models in which we varied the number of thermal pulses, the amount of overshooting, and the 12C( ; )16O reaction rate within their uncertainties. Results. We explore the impact of these major uncertainties in prior evolution on the chemical structure and expected pulsation spectrum. We find that these uncertainties yield significant changes in the g-mode pulsation periods. Conclusions. We conclude that the uncertainties in the white dwarf progenitor evolution should be taken into account in detailed asteroseismological analyses of these pulsating stars.application/pdfengAstronomy and astrophysics. Les Ulis. Vol. 599 (Mar. 2017), A21, 7 p.AsterosismologiaEstrelas ZZ CetiAnãs brancasEvolucao estelarPulsacoes estelaresAsteroseismologyStars: evolutionWhite dwarfsStars: oscillationsAsteroseismology of ZZ Ceti stars with fully evolutionary white dwarf models : I. the impact of the uncertainties from prior evolution on the period spectrumEstrangeiroinfo: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:UFRGSORIGINAL001063756.pdf001063756.pdfTexto completo (inglês)application/pdf355215http://www.lume.ufrgs.br/bitstream/10183/175042/1/001063756.pdfde8d496a037a5a99f793d7e63ee312eaMD51TEXT001063756.pdf.txt001063756.pdf.txtExtracted Texttext/plain35279http://www.lume.ufrgs.br/bitstream/10183/175042/2/001063756.pdf.txtdca38db1c894f50d192ff20d9d2dc75fMD52THUMBNAIL001063756.pdf.jpg001063756.pdf.jpgGenerated Thumbnailimage/jpeg1899http://www.lume.ufrgs.br/bitstream/10183/175042/3/001063756.pdf.jpg5fe53154971fa53524768e87dfcef719MD5310183/1750422023-05-14 03:24:35.269717oai:www.lume.ufrgs.br:10183/175042Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-05-14T06:24:35Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Asteroseismology of ZZ Ceti stars with fully evolutionary white dwarf models : I. the impact of the uncertainties from prior evolution on the period spectrum |
title |
Asteroseismology of ZZ Ceti stars with fully evolutionary white dwarf models : I. the impact of the uncertainties from prior evolution on the period spectrum |
spellingShingle |
Asteroseismology of ZZ Ceti stars with fully evolutionary white dwarf models : I. the impact of the uncertainties from prior evolution on the period spectrum De Gerónimo, Francisco Cesar Asterosismologia Estrelas ZZ Ceti Anãs brancas Evolucao estelar Pulsacoes estelares Asteroseismology Stars: evolution White dwarfs Stars: oscillations |
title_short |
Asteroseismology of ZZ Ceti stars with fully evolutionary white dwarf models : I. the impact of the uncertainties from prior evolution on the period spectrum |
title_full |
Asteroseismology of ZZ Ceti stars with fully evolutionary white dwarf models : I. the impact of the uncertainties from prior evolution on the period spectrum |
title_fullStr |
Asteroseismology of ZZ Ceti stars with fully evolutionary white dwarf models : I. the impact of the uncertainties from prior evolution on the period spectrum |
title_full_unstemmed |
Asteroseismology of ZZ Ceti stars with fully evolutionary white dwarf models : I. the impact of the uncertainties from prior evolution on the period spectrum |
title_sort |
Asteroseismology of ZZ Ceti stars with fully evolutionary white dwarf models : I. the impact of the uncertainties from prior evolution on the period spectrum |
author |
De Gerónimo, Francisco Cesar |
author_facet |
De Gerónimo, Francisco Cesar Althaus, Leandro Gabriel Córsico, Alejandro Hugo Romero, Alejandra Daniela Kepler, Souza Oliveira |
author_role |
author |
author2 |
Althaus, Leandro Gabriel Córsico, Alejandro Hugo Romero, Alejandra Daniela Kepler, Souza Oliveira |
author2_role |
author author author author |
dc.contributor.author.fl_str_mv |
De Gerónimo, Francisco Cesar Althaus, Leandro Gabriel Córsico, Alejandro Hugo Romero, Alejandra Daniela Kepler, Souza Oliveira |
dc.subject.por.fl_str_mv |
Asterosismologia Estrelas ZZ Ceti Anãs brancas Evolucao estelar Pulsacoes estelares |
topic |
Asterosismologia Estrelas ZZ Ceti Anãs brancas Evolucao estelar Pulsacoes estelares Asteroseismology Stars: evolution White dwarfs Stars: oscillations |
dc.subject.eng.fl_str_mv |
Asteroseismology Stars: evolution White dwarfs Stars: oscillations |
description |
Context. ZZ Ceti stars are pulsating white dwarfs with a carbon-oxygen core build up during the core helium burning and thermally pulsing Asymptotic Giant Branch phases. Through the interpretation of their pulsation periods by means of asteroseismology, details about their origin and evolution can be inferred. The whole pulsation spectrum exhibited by ZZ Ceti stars strongly depends on the inner chemical structure. At present, there are several processes a ecting the chemical profiles that are still not accurately determined. Aims. We present a study of the impact of the current uncertainties of the white dwarf formation and evolution on the expected pulsation properties of ZZ Ceti stars. Methods. Our analysis is based on a set of carbon-oxygen core white dwarf models with masses 0:548 and 0:837 M that are derived from full evolutionary computations from the ZAMS to the ZZ Ceti domain. We considered models in which we varied the number of thermal pulses, the amount of overshooting, and the 12C( ; )16O reaction rate within their uncertainties. Results. We explore the impact of these major uncertainties in prior evolution on the chemical structure and expected pulsation spectrum. We find that these uncertainties yield significant changes in the g-mode pulsation periods. Conclusions. We conclude that the uncertainties in the white dwarf progenitor evolution should be taken into account in detailed asteroseismological analyses of these pulsating stars. |
publishDate |
2017 |
dc.date.issued.fl_str_mv |
2017 |
dc.date.accessioned.fl_str_mv |
2018-04-26T02:33:00Z |
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http://hdl.handle.net/10183/175042 |
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0004-6361 |
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001063756 |
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dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy and astrophysics. Les Ulis. Vol. 599 (Mar. 2017), A21, 7 p. |
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openAccess |
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