Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501

Autores
Córsico, Alejandro Hugo; Althaus, Leandro Gabriel; Miller Bertolami, Marcelo Miguel; García Berro, E.
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. We present an asteroseismological study on the two high-gravity pulsating PG 1159 (GW Vir or DOV) stars, PG 2131+066 and PG 1707+427, and on the pulsating [WCE] star NGC 1501. All of these stars have been intensively scrutinized through multi-site observations, so they have well resolved pulsation spectra.Methods. We compute adiabatic g-mode pulsation periods on PG 1159 evolutionary models with stellar masses ranging from 0.530 to 0.741M. These models take into account the complete evolution of progenitor stars, through the thermally pulsing AGB phase, and born-again episode. We constrain the stellar mass of PG 2131+066, PG 1707+427, and NGC 1501 by comparing the observed period spacing with the asymptotic period spacing and with the average of the computed period spacings. We also employ the individual observed periods in search of representative seismological models for each star.Results. We derive a stellar mass of 0.627 M for PG 2131+066, 0.597 M for PG 1707+427, and 0.571 M for NGC 1501 from a comparison between the observed period spacings and the computed asymptotic period spacings, and a stellar mass of 0.627 M for PG 2131+066, 0.597 M for PG 1707+427, and 0.571 M for NGC 1501 by comparing the observed period spacings with the average of the computed period spacings. We also find, on the basis of a period-fit procedure, asteroseismological models representatives of PG 2131+066 and PG 1707+427. These best-fit models are able to reproduce the observed period patterns of these stars with an average of the period differences of δII=1.57 s and δII 1.75 s, respectively. The best-fit model for PG 2131+066 has an effective temperature Teff = 102 100 K, a stellar mass M = 0.589 M, a surface gravity logg = 7.63, a stellar luminosity and radius of log(L/L) = 1.57 and log(R/R) = -1.71, respectively, and a He-rich envelope thickness of Menv = 1.6 10-2 M. We derive a seismic distance d ̃ 830 pc and a parallax π ̃ 1.2 mas. The best-fit model for PG 1707+427, on the other hand, has Teff = 89 500 K, M = 0.542 M, logg = 7.53, log(L/L) = 1.40, log(R/R) = -1.68, and Menv = 2.5 10-2 M, and the seismic distance and parallax are d ̃ 730 pc and π ̃ 1.4 mas. Finally, we have been unable to find an unambiguous best-fit model for NGC 1501 on the basis of a period-fit procedure.Conclusions. This work closes our short series of asteroseismological studies on pulsating pre-white dwarf stars. Our results demonstrate the usefulness of asteroseismology for probing the internal structure and evolutionary status of pre-white dwarf stars. In particular, asteroseismology is able to determine stellar masses of PG 1159 stars with an accuracy comparable or even better than spectroscopy.
Instituto de Astrofísica de La Plata
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
Stars: evolution
Stars: interiors
Stars: oscillations
White dwarfs
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/82676

id SEDICI_06ad5855dd3800f76d43352c0cabb097
oai_identifier_str oai:sedici.unlp.edu.ar:10915/82676
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501Córsico, Alejandro HugoAlthaus, Leandro GabrielMiller Bertolami, Marcelo MiguelGarcía Berro, E.Ciencias AstronómicasStars: evolutionStars: interiorsStars: oscillationsWhite dwarfsAims. We present an asteroseismological study on the two high-gravity pulsating PG 1159 (GW Vir or DOV) stars, PG 2131+066 and PG 1707+427, and on the pulsating [WCE] star NGC 1501. All of these stars have been intensively scrutinized through multi-site observations, so they have well resolved pulsation spectra.Methods. We compute adiabatic g-mode pulsation periods on PG 1159 evolutionary models with stellar masses ranging from 0.530 to 0.741M. These models take into account the complete evolution of progenitor stars, through the thermally pulsing AGB phase, and born-again episode. We constrain the stellar mass of PG 2131+066, PG 1707+427, and NGC 1501 by comparing the observed period spacing with the asymptotic period spacing and with the average of the computed period spacings. We also employ the individual observed periods in search of representative seismological models for each star.Results. We derive a stellar mass of 0.627 M for PG 2131+066, 0.597 M for PG 1707+427, and 0.571 M for NGC 1501 from a comparison between the observed period spacings and the computed asymptotic period spacings, and a stellar mass of 0.627 M for PG 2131+066, 0.597 M for PG 1707+427, and 0.571 M for NGC 1501 by comparing the observed period spacings with the average of the computed period spacings. We also find, on the basis of a period-fit procedure, asteroseismological models representatives of PG 2131+066 and PG 1707+427. These best-fit models are able to reproduce the observed period patterns of these stars with an average of the period differences of δII=1.57 s and δII 1.75 s, respectively. The best-fit model for PG 2131+066 has an effective temperature Teff = 102 100 K, a stellar mass M = 0.589 M, a surface gravity logg = 7.63, a stellar luminosity and radius of log(L/L) = 1.57 and log(R/R) = -1.71, respectively, and a He-rich envelope thickness of Menv = 1.6 10-2 M. We derive a seismic distance d ̃ 830 pc and a parallax π ̃ 1.2 mas. The best-fit model for PG 1707+427, on the other hand, has Teff = 89 500 K, M = 0.542 M, logg = 7.53, log(L/L) = 1.40, log(R/R) = -1.68, and Menv = 2.5 10-2 M, and the seismic distance and parallax are d ̃ 730 pc and π ̃ 1.4 mas. Finally, we have been unable to find an unambiguous best-fit model for NGC 1501 on the basis of a period-fit procedure.Conclusions. This work closes our short series of asteroseismological studies on pulsating pre-white dwarf stars. Our results demonstrate the usefulness of asteroseismology for probing the internal structure and evolutionary status of pre-white dwarf stars. In particular, asteroseismology is able to determine stellar masses of PG 1159 stars with an accuracy comparable or even better than spectroscopy.Instituto de Astrofísica de La PlataFacultad de Ciencias Astronómicas y Geofísicas2009info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf257-266http://sedici.unlp.edu.ar/handle/10915/82676enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200810727info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:15:36Zoai:sedici.unlp.edu.ar:10915/82676Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:15:36.35SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501
title Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501
spellingShingle Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501
Córsico, Alejandro Hugo
Ciencias Astronómicas
Stars: evolution
Stars: interiors
Stars: oscillations
White dwarfs
title_short Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501
title_full Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501
title_fullStr Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501
title_full_unstemmed Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501
title_sort Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501
dc.creator.none.fl_str_mv Córsico, Alejandro Hugo
Althaus, Leandro Gabriel
Miller Bertolami, Marcelo Miguel
García Berro, E.
author Córsico, Alejandro Hugo
author_facet Córsico, Alejandro Hugo
Althaus, Leandro Gabriel
Miller Bertolami, Marcelo Miguel
García Berro, E.
author_role author
author2 Althaus, Leandro Gabriel
Miller Bertolami, Marcelo Miguel
García Berro, E.
author2_role author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Stars: evolution
Stars: interiors
Stars: oscillations
White dwarfs
topic Ciencias Astronómicas
Stars: evolution
Stars: interiors
Stars: oscillations
White dwarfs
dc.description.none.fl_txt_mv Aims. We present an asteroseismological study on the two high-gravity pulsating PG 1159 (GW Vir or DOV) stars, PG 2131+066 and PG 1707+427, and on the pulsating [WCE] star NGC 1501. All of these stars have been intensively scrutinized through multi-site observations, so they have well resolved pulsation spectra.Methods. We compute adiabatic g-mode pulsation periods on PG 1159 evolutionary models with stellar masses ranging from 0.530 to 0.741M. These models take into account the complete evolution of progenitor stars, through the thermally pulsing AGB phase, and born-again episode. We constrain the stellar mass of PG 2131+066, PG 1707+427, and NGC 1501 by comparing the observed period spacing with the asymptotic period spacing and with the average of the computed period spacings. We also employ the individual observed periods in search of representative seismological models for each star.Results. We derive a stellar mass of 0.627 M for PG 2131+066, 0.597 M for PG 1707+427, and 0.571 M for NGC 1501 from a comparison between the observed period spacings and the computed asymptotic period spacings, and a stellar mass of 0.627 M for PG 2131+066, 0.597 M for PG 1707+427, and 0.571 M for NGC 1501 by comparing the observed period spacings with the average of the computed period spacings. We also find, on the basis of a period-fit procedure, asteroseismological models representatives of PG 2131+066 and PG 1707+427. These best-fit models are able to reproduce the observed period patterns of these stars with an average of the period differences of δII=1.57 s and δII 1.75 s, respectively. The best-fit model for PG 2131+066 has an effective temperature Teff = 102 100 K, a stellar mass M = 0.589 M, a surface gravity logg = 7.63, a stellar luminosity and radius of log(L/L) = 1.57 and log(R/R) = -1.71, respectively, and a He-rich envelope thickness of Menv = 1.6 10-2 M. We derive a seismic distance d ̃ 830 pc and a parallax π ̃ 1.2 mas. The best-fit model for PG 1707+427, on the other hand, has Teff = 89 500 K, M = 0.542 M, logg = 7.53, log(L/L) = 1.40, log(R/R) = -1.68, and Menv = 2.5 10-2 M, and the seismic distance and parallax are d ̃ 730 pc and π ̃ 1.4 mas. Finally, we have been unable to find an unambiguous best-fit model for NGC 1501 on the basis of a period-fit procedure.Conclusions. This work closes our short series of asteroseismological studies on pulsating pre-white dwarf stars. Our results demonstrate the usefulness of asteroseismology for probing the internal structure and evolutionary status of pre-white dwarf stars. In particular, asteroseismology is able to determine stellar masses of PG 1159 stars with an accuracy comparable or even better than spectroscopy.
Instituto de Astrofísica de La Plata
Facultad de Ciencias Astronómicas y Geofísicas
description Aims. We present an asteroseismological study on the two high-gravity pulsating PG 1159 (GW Vir or DOV) stars, PG 2131+066 and PG 1707+427, and on the pulsating [WCE] star NGC 1501. All of these stars have been intensively scrutinized through multi-site observations, so they have well resolved pulsation spectra.Methods. We compute adiabatic g-mode pulsation periods on PG 1159 evolutionary models with stellar masses ranging from 0.530 to 0.741M. These models take into account the complete evolution of progenitor stars, through the thermally pulsing AGB phase, and born-again episode. We constrain the stellar mass of PG 2131+066, PG 1707+427, and NGC 1501 by comparing the observed period spacing with the asymptotic period spacing and with the average of the computed period spacings. We also employ the individual observed periods in search of representative seismological models for each star.Results. We derive a stellar mass of 0.627 M for PG 2131+066, 0.597 M for PG 1707+427, and 0.571 M for NGC 1501 from a comparison between the observed period spacings and the computed asymptotic period spacings, and a stellar mass of 0.627 M for PG 2131+066, 0.597 M for PG 1707+427, and 0.571 M for NGC 1501 by comparing the observed period spacings with the average of the computed period spacings. We also find, on the basis of a period-fit procedure, asteroseismological models representatives of PG 2131+066 and PG 1707+427. These best-fit models are able to reproduce the observed period patterns of these stars with an average of the period differences of δII=1.57 s and δII 1.75 s, respectively. The best-fit model for PG 2131+066 has an effective temperature Teff = 102 100 K, a stellar mass M = 0.589 M, a surface gravity logg = 7.63, a stellar luminosity and radius of log(L/L) = 1.57 and log(R/R) = -1.71, respectively, and a He-rich envelope thickness of Menv = 1.6 10-2 M. We derive a seismic distance d ̃ 830 pc and a parallax π ̃ 1.2 mas. The best-fit model for PG 1707+427, on the other hand, has Teff = 89 500 K, M = 0.542 M, logg = 7.53, log(L/L) = 1.40, log(R/R) = -1.68, and Menv = 2.5 10-2 M, and the seismic distance and parallax are d ̃ 730 pc and π ̃ 1.4 mas. Finally, we have been unable to find an unambiguous best-fit model for NGC 1501 on the basis of a period-fit procedure.Conclusions. This work closes our short series of asteroseismological studies on pulsating pre-white dwarf stars. Our results demonstrate the usefulness of asteroseismology for probing the internal structure and evolutionary status of pre-white dwarf stars. In particular, asteroseismology is able to determine stellar masses of PG 1159 stars with an accuracy comparable or even better than spectroscopy.
publishDate 2009
dc.date.none.fl_str_mv 2009
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/82676
url http://sedici.unlp.edu.ar/handle/10915/82676
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-6361
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200810727
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
257-266
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instname:Universidad Nacional de La Plata
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repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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