Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47

Autores
Calcaferro, Leila Magdalena; Corsico, Alejandro Hugo; Althaus, Leandro Gabriel
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. GW Virginis stars are a well-studied class of nonradial g-mode pulsators. SDSS J0349−0059 and VV 47 are two PG 1159 star members of this class of variable stars. SDSS J0349−0059 is an interesting GW Vir star that shows a complete pulsation spectrum that includes rotational splitting of some of its frequencies. VV 47 is a pulsating PG 1159 star surrounded by a planetary nebula. This star is particularly interesting because it exhibits a rich and complex pulsation spectrum.Aims. We present an asteroseismological study of SDSS J0349−0059 and VV 47 aimed mainly at deriving their total mass on the basis of state-of-the-art PG 1159 evolutionary models.Methods. We computed adiabatic nonradial g-mode pulsation periods for PG 1159 evolutionary models with stellar masses ranging from 0.515 to 0.741 M⊙, that take into account the complete evolution of the progenitor stars. We first estimated a mean period spacing for both SDSS J0349−0059 and VV 47 and then constrained the stellar mass of these stars 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 to search for a representative seismological model for each star. Finally, we estimated the rotation period of SDSS J0349−0059.Results. We found a spectroscopic mass of M⋆ ~ 0.543 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.529 M⊙ for VV 47. By comparing the observed period spacing with the asymptotic period spacing, we obtain M⋆ ~ 0.569 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.523 M⊙ for VV 47. When we compare the observed period spacing with the average of the computed period spacings, we find M⋆ ~ 0.535 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.528 M⊙ for VV 47. Searching for the best period fit, we found for SDSS J0349−0059 an asteroseismological model with M⋆ = 0.542 M⊙ and Teff = 91 255 K. For VV 47, we were unable to find a unique and unambiguous asteroseismological model. Finally, for SDSS J0349−0059, we determined the rotation period to be Prot = 1/Ω ~ 0.407 days.Conclusions. The results presented in this work constitute a further step in the study of GW Vir stars through asteroseismology in the frame of fully evolutionary models of PG 1159 stars. In particular, the potential of asteroseismology to derive stellar masses of PG 1159 stars with an unprecedented precision is shown yet again.
Fil: Calcaferro, Leila Magdalena. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
Fil: Corsico, Alejandro Hugo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
Fil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
Materia
Evolution of stars
Interior stars
Oscillations
White dwarfs
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/35731

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network_name_str CONICET Digital (CONICET)
spelling Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47Calcaferro, Leila MagdalenaCorsico, Alejandro HugoAlthaus, Leandro GabrielEvolution of starsInterior starsOscillationsWhite dwarfshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. GW Virginis stars are a well-studied class of nonradial g-mode pulsators. SDSS J0349−0059 and VV 47 are two PG 1159 star members of this class of variable stars. SDSS J0349−0059 is an interesting GW Vir star that shows a complete pulsation spectrum that includes rotational splitting of some of its frequencies. VV 47 is a pulsating PG 1159 star surrounded by a planetary nebula. This star is particularly interesting because it exhibits a rich and complex pulsation spectrum.Aims. We present an asteroseismological study of SDSS J0349−0059 and VV 47 aimed mainly at deriving their total mass on the basis of state-of-the-art PG 1159 evolutionary models.Methods. We computed adiabatic nonradial g-mode pulsation periods for PG 1159 evolutionary models with stellar masses ranging from 0.515 to 0.741 M⊙, that take into account the complete evolution of the progenitor stars. We first estimated a mean period spacing for both SDSS J0349−0059 and VV 47 and then constrained the stellar mass of these stars 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 to search for a representative seismological model for each star. Finally, we estimated the rotation period of SDSS J0349−0059.Results. We found a spectroscopic mass of M⋆ ~ 0.543 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.529 M⊙ for VV 47. By comparing the observed period spacing with the asymptotic period spacing, we obtain M⋆ ~ 0.569 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.523 M⊙ for VV 47. When we compare the observed period spacing with the average of the computed period spacings, we find M⋆ ~ 0.535 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.528 M⊙ for VV 47. Searching for the best period fit, we found for SDSS J0349−0059 an asteroseismological model with M⋆ = 0.542 M⊙ and Teff = 91 255 K. For VV 47, we were unable to find a unique and unambiguous asteroseismological model. Finally, for SDSS J0349−0059, we determined the rotation period to be Prot = 1/Ω ~ 0.407 days.Conclusions. The results presented in this work constitute a further step in the study of GW Vir stars through asteroseismology in the frame of fully evolutionary models of PG 1159 stars. In particular, the potential of asteroseismology to derive stellar masses of PG 1159 stars with an unprecedented precision is shown yet again.Fil: Calcaferro, Leila Magdalena. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; ArgentinaFil: Corsico, Alejandro Hugo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; ArgentinaFil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; ArgentinaEDP Sciences2016-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/35731Calcaferro, Leila Magdalena; Corsico, Alejandro Hugo; Althaus, Leandro Gabriel; Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47; EDP Sciences; Astronomy and Astrophysics; 589; 4-20160004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201527996info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2016/05/aa27996-15/aa27996-15.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:00:27Zoai:ri.conicet.gov.ar:11336/35731instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:00:27.635CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47
title Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47
spellingShingle Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47
Calcaferro, Leila Magdalena
Evolution of stars
Interior stars
Oscillations
White dwarfs
title_short Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47
title_full Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47
title_fullStr Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47
title_full_unstemmed Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47
title_sort Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47
dc.creator.none.fl_str_mv Calcaferro, Leila Magdalena
Corsico, Alejandro Hugo
Althaus, Leandro Gabriel
author Calcaferro, Leila Magdalena
author_facet Calcaferro, Leila Magdalena
Corsico, Alejandro Hugo
Althaus, Leandro Gabriel
author_role author
author2 Corsico, Alejandro Hugo
Althaus, Leandro Gabriel
author2_role author
author
dc.subject.none.fl_str_mv Evolution of stars
Interior stars
Oscillations
White dwarfs
topic Evolution of stars
Interior stars
Oscillations
White dwarfs
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. GW Virginis stars are a well-studied class of nonradial g-mode pulsators. SDSS J0349−0059 and VV 47 are two PG 1159 star members of this class of variable stars. SDSS J0349−0059 is an interesting GW Vir star that shows a complete pulsation spectrum that includes rotational splitting of some of its frequencies. VV 47 is a pulsating PG 1159 star surrounded by a planetary nebula. This star is particularly interesting because it exhibits a rich and complex pulsation spectrum.Aims. We present an asteroseismological study of SDSS J0349−0059 and VV 47 aimed mainly at deriving their total mass on the basis of state-of-the-art PG 1159 evolutionary models.Methods. We computed adiabatic nonradial g-mode pulsation periods for PG 1159 evolutionary models with stellar masses ranging from 0.515 to 0.741 M⊙, that take into account the complete evolution of the progenitor stars. We first estimated a mean period spacing for both SDSS J0349−0059 and VV 47 and then constrained the stellar mass of these stars 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 to search for a representative seismological model for each star. Finally, we estimated the rotation period of SDSS J0349−0059.Results. We found a spectroscopic mass of M⋆ ~ 0.543 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.529 M⊙ for VV 47. By comparing the observed period spacing with the asymptotic period spacing, we obtain M⋆ ~ 0.569 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.523 M⊙ for VV 47. When we compare the observed period spacing with the average of the computed period spacings, we find M⋆ ~ 0.535 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.528 M⊙ for VV 47. Searching for the best period fit, we found for SDSS J0349−0059 an asteroseismological model with M⋆ = 0.542 M⊙ and Teff = 91 255 K. For VV 47, we were unable to find a unique and unambiguous asteroseismological model. Finally, for SDSS J0349−0059, we determined the rotation period to be Prot = 1/Ω ~ 0.407 days.Conclusions. The results presented in this work constitute a further step in the study of GW Vir stars through asteroseismology in the frame of fully evolutionary models of PG 1159 stars. In particular, the potential of asteroseismology to derive stellar masses of PG 1159 stars with an unprecedented precision is shown yet again.
Fil: Calcaferro, Leila Magdalena. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
Fil: Corsico, Alejandro Hugo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
Fil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
description Context. GW Virginis stars are a well-studied class of nonradial g-mode pulsators. SDSS J0349−0059 and VV 47 are two PG 1159 star members of this class of variable stars. SDSS J0349−0059 is an interesting GW Vir star that shows a complete pulsation spectrum that includes rotational splitting of some of its frequencies. VV 47 is a pulsating PG 1159 star surrounded by a planetary nebula. This star is particularly interesting because it exhibits a rich and complex pulsation spectrum.Aims. We present an asteroseismological study of SDSS J0349−0059 and VV 47 aimed mainly at deriving their total mass on the basis of state-of-the-art PG 1159 evolutionary models.Methods. We computed adiabatic nonradial g-mode pulsation periods for PG 1159 evolutionary models with stellar masses ranging from 0.515 to 0.741 M⊙, that take into account the complete evolution of the progenitor stars. We first estimated a mean period spacing for both SDSS J0349−0059 and VV 47 and then constrained the stellar mass of these stars 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 to search for a representative seismological model for each star. Finally, we estimated the rotation period of SDSS J0349−0059.Results. We found a spectroscopic mass of M⋆ ~ 0.543 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.529 M⊙ for VV 47. By comparing the observed period spacing with the asymptotic period spacing, we obtain M⋆ ~ 0.569 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.523 M⊙ for VV 47. When we compare the observed period spacing with the average of the computed period spacings, we find M⋆ ~ 0.535 M⊙ for SDSS J0349−0059 and M⋆ ~ 0.528 M⊙ for VV 47. Searching for the best period fit, we found for SDSS J0349−0059 an asteroseismological model with M⋆ = 0.542 M⊙ and Teff = 91 255 K. For VV 47, we were unable to find a unique and unambiguous asteroseismological model. Finally, for SDSS J0349−0059, we determined the rotation period to be Prot = 1/Ω ~ 0.407 days.Conclusions. The results presented in this work constitute a further step in the study of GW Vir stars through asteroseismology in the frame of fully evolutionary models of PG 1159 stars. In particular, the potential of asteroseismology to derive stellar masses of PG 1159 stars with an unprecedented precision is shown yet again.
publishDate 2016
dc.date.none.fl_str_mv 2016-04
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
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info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/35731
Calcaferro, Leila Magdalena; Corsico, Alejandro Hugo; Althaus, Leandro Gabriel; Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47; EDP Sciences; Astronomy and Astrophysics; 589; 4-2016
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/35731
identifier_str_mv Calcaferro, Leila Magdalena; Corsico, Alejandro Hugo; Althaus, Leandro Gabriel; Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47; EDP Sciences; Astronomy and Astrophysics; 589; 4-2016
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
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info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2016/05/aa27996-15/aa27996-15.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
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instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
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