The pulsation modes of the pre-white dwarf PG 1159-035

Autores
Costa, J. E. S.; Kepler, S. O.; Winget, D. E.; O'Brien, M. S.; Kawaler, S. D.; Costa, A. F. M.; Giovannini, O.; Kanaan, A.; Mukadam, A. S.; Mullally, F.; Nitta, A.; Provençal, J. L.; Shipman, H.; Wood, M. A.; Ahrens, T. J.; Grauer, A.; Kilic, M.; Bradley, P. A.; Sekiguchi, K.; Crowe, R.; Jiang, X. J.; Sullivan, D.; Sullivan, T.; Rosen, R.; Clemens, J. C.; Janulis, R.; O'Donoghue, D.; Ogloza, W.; Baran, A.; Silvotti, R.; Marinoni, S.; Vauclair, G.; Dolez, N.; Chevreton, M.; Dreizler, S.; Schuh, S.; Deetjen, J.; Nagel, T.; Solheim, J.-E.; González Pérez, J. M.; Althaus, Leandro Gabriel; Corsico, Alejandro Hugo
Año de publicación
2008
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context.PG 1159-035, a pre-white dwarf with 140 000 K, is the prototype of both two classes: the PG 1159 spectroscopic class and the DOV pulsating class. Previous studies of PG 1159-035 photometric data obtained with the Whole Earth Telescope (WET) showed a rich frequency spectrum allowing the identification of 122 pulsation modes. Analyzing the periods of pulsation, it is possible to measure the stellar mass, the rotational period and the inclination of the rotation axis, to estimate an upper limit for the magnetic field, and even to obtain information about the inner stratification of the star. Aims.We have three principal aims: to increase the number of detected and identified pulsation modes in PG 1159-035, study trapping of the star's pulsation modes, and to improve or constrain the determination of stellar parameters. Methods.We used all available WET photometric data from 1983, 1985, 1989, 1993 and 2002 to identify the pulsation periods. Results.We identified 76 additional pulsation modes, increasing to 198 the number of known pulsation modes in PG 1159-035, the largest number of modes detected in any star besides the Sun. From the period spacing we estimated a mass = 0.59 ± 0.02 for PG 1159-035, with the uncertainty dominated by the models, not the observation. Deviations in the regular period spacing suggest that some of the pulsation modes are trapped, even though the star is a pre-white dwarf and the gravitational settling is ongoing. The position of the transition zone that causes the mode trapping was calculated at = 0.83 ± 0.05. From the multiplet splitting, we calculated the rotational period Prot = 1.3920 ± 0.0008 days and an upper limit for the magnetic field, G. The total power of the pulsation modes at the stellar surface changed less than 30% for = 1 modes and less than 50% for = 2 modes. We find no evidence of linear combinations between the 198 pulsation mode frequencies. PG 1159-035 models have not significative convection zones, supporting the hypothesis that nonlinearity arises in the convection zones in cooler pulsating white dwarf stars.
Fil: Costa, J. E. S.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Kepler, S. O.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Winget, D. E.. University of Texas at Austin; Estados Unidos
Fil: O'Brien, M. S.. University of Yale; Estados Unidos
Fil: Kawaler, S. D.. Iowa Steate University; Estados Unidos
Fil: Costa, A. F. M.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Giovannini, O.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Kanaan, A.. Universidade Federal de Santa Catarina; Brasil
Fil: Mukadam, A. S.. University of Washington; Estados Unidos
Fil: Mullally, F.. University of Texas at Austin; Estados Unidos
Fil: Nitta, A.. Gemini Observatory; Estados Unidos
Fil: Provençal, J. L.. University of Delaware; Estados Unidos
Fil: Shipman, H.. University of Delaware; Estados Unidos
Fil: Wood, M. A.. Florida Institute of Technology; Estados Unidos
Fil: Ahrens, T. J.. Florida Institute of Technology; Estados Unidos
Fil: Grauer, A.. University of Arkansas at Little Rock; Estados Unidos
Fil: Kilic, M.. Ohio State University; Estados Unidos
Fil: Bradley, P. A.. Los Alamos National Laboratory; Estados Unidos
Fil: Sekiguchi, K.. Subaru National Astronomical Observatory of Japan; Japón
Fil: Crowe, R.. University of Hawaii; Estados Unidos
Fil: Jiang, X. J.. Chinese Academy of Sciences; República de China
Fil: Sullivan, D.. University of Victoria; Nueva Zelanda
Fil: Sullivan, T.. University of Victoria; Nueva Zelanda
Fil: Rosen, R.. University of Victoria; Nueva Zelanda
Fil: Clemens, J. C.. University of North Carolina; Estados Unidos
Fil: Janulis, R.. VU Institute of Theoretical Physics and Astronomy; Lituania
Fil: O'Donoghue, D.. South African Astronomical Observatory; Sudáfrica
Fil: Ogloza, W.. Cracow Pedagogical University; Polonia
Fil: Baran, A.. Cracow Pedagogical University; Polonia
Fil: Silvotti, R.. Osservatorio Astronomico di Capodimonte; Italia
Fil: Marinoni, S.. Osservatorio Astronomico di Bologna; Italia
Fil: Vauclair, G.. Université Paul Sabatier; Francia
Fil: Dolez, N.. Université Paul Sabatier; Francia
Fil: Chevreton, M.. Observatoire de Paris-Meudon; Francia
Fil: Dreizler, S.. Institut für Astrophysik; Alemania
Fil: Schuh, S.. Institut für Astrophysik; Alemania
Fil: Deetjen, J.. Institut für Astrophysik; Alemania
Fil: Nagel, T.. Institut für Astrophysik; Alemania
Fil: Solheim, J.-E.. Universitetet i Tromsø; Noruega
Fil: González Pérez, J. M.. Universitetet i Tromsø; Noruega
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
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
Materia
Oscillations
PG 1159-035 (estrella)
Interior stars
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:11336/44898
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/44898
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repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The pulsation modes of the pre-white dwarf PG 1159-035Costa, J. E. S.Kepler, S. O.Winget, D. E.O'Brien, M. S.Kawaler, S. D.Costa, A. F. M.Giovannini, O.Kanaan, A.Mukadam, A. S.Mullally, F.Nitta, A.Provençal, J. L.Shipman, H.Wood, M. A.Ahrens, T. J.Grauer, A.Kilic, M.Bradley, P. A.Sekiguchi, K.Crowe, R.Jiang, X. J.Sullivan, D.Sullivan, T.Rosen, R.Clemens, J. C.Janulis, R.O'Donoghue, D.Ogloza, W.Baran, A.Silvotti, R.Marinoni, S.Vauclair, G.Dolez, N.Chevreton, M.Dreizler, S.Schuh, S.Deetjen, J.Nagel, T.Solheim, J.-E.González Pérez, J. M.Althaus, Leandro GabrielCorsico, Alejandro HugoOscillationsPG 1159-035 (estrella)Interior starsWhite dwarfshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context.PG 1159-035, a pre-white dwarf with 140 000 K, is the prototype of both two classes: the PG 1159 spectroscopic class and the DOV pulsating class. Previous studies of PG 1159-035 photometric data obtained with the Whole Earth Telescope (WET) showed a rich frequency spectrum allowing the identification of 122 pulsation modes. Analyzing the periods of pulsation, it is possible to measure the stellar mass, the rotational period and the inclination of the rotation axis, to estimate an upper limit for the magnetic field, and even to obtain information about the inner stratification of the star. Aims.We have three principal aims: to increase the number of detected and identified pulsation modes in PG 1159-035, study trapping of the star's pulsation modes, and to improve or constrain the determination of stellar parameters. Methods.We used all available WET photometric data from 1983, 1985, 1989, 1993 and 2002 to identify the pulsation periods. Results.We identified 76 additional pulsation modes, increasing to 198 the number of known pulsation modes in PG 1159-035, the largest number of modes detected in any star besides the Sun. From the period spacing we estimated a mass = 0.59 ± 0.02 for PG 1159-035, with the uncertainty dominated by the models, not the observation. Deviations in the regular period spacing suggest that some of the pulsation modes are trapped, even though the star is a pre-white dwarf and the gravitational settling is ongoing. The position of the transition zone that causes the mode trapping was calculated at = 0.83 ± 0.05. From the multiplet splitting, we calculated the rotational period Prot = 1.3920 ± 0.0008 days and an upper limit for the magnetic field, G. The total power of the pulsation modes at the stellar surface changed less than 30% for = 1 modes and less than 50% for = 2 modes. We find no evidence of linear combinations between the 198 pulsation mode frequencies. PG 1159-035 models have not significative convection zones, supporting the hypothesis that nonlinearity arises in the convection zones in cooler pulsating white dwarf stars.Fil: Costa, J. E. S.. Universidade Federal do Rio Grande do Sul; BrasilFil: Kepler, S. O.. Universidade Federal do Rio Grande do Sul; BrasilFil: Winget, D. E.. University of Texas at Austin; Estados UnidosFil: O'Brien, M. S.. University of Yale; Estados UnidosFil: Kawaler, S. D.. Iowa Steate University; Estados UnidosFil: Costa, A. F. M.. Universidade Federal do Rio Grande do Sul; BrasilFil: Giovannini, O.. Universidade Federal do Rio Grande do Sul; BrasilFil: Kanaan, A.. Universidade Federal de Santa Catarina; BrasilFil: Mukadam, A. S.. University of Washington; Estados UnidosFil: Mullally, F.. University of Texas at Austin; Estados UnidosFil: Nitta, A.. Gemini Observatory; Estados UnidosFil: Provençal, J. L.. University of Delaware; Estados UnidosFil: Shipman, H.. University of Delaware; Estados UnidosFil: Wood, M. A.. Florida Institute of Technology; Estados UnidosFil: Ahrens, T. J.. Florida Institute of Technology; Estados UnidosFil: Grauer, A.. University of Arkansas at Little Rock; Estados UnidosFil: Kilic, M.. Ohio State University; Estados UnidosFil: Bradley, P. A.. Los Alamos National Laboratory; Estados UnidosFil: Sekiguchi, K.. Subaru National Astronomical Observatory of Japan; JapónFil: Crowe, R.. University of Hawaii; Estados UnidosFil: Jiang, X. J.. Chinese Academy of Sciences; República de ChinaFil: Sullivan, D.. University of Victoria; Nueva ZelandaFil: Sullivan, T.. University of Victoria; Nueva ZelandaFil: Rosen, R.. University of Victoria; Nueva ZelandaFil: Clemens, J. C.. University of North Carolina; Estados UnidosFil: Janulis, R.. VU Institute of Theoretical Physics and Astronomy; LituaniaFil: O'Donoghue, D.. South African Astronomical Observatory; SudáfricaFil: Ogloza, W.. Cracow Pedagogical University; PoloniaFil: Baran, A.. Cracow Pedagogical University; PoloniaFil: Silvotti, R.. Osservatorio Astronomico di Capodimonte; ItaliaFil: Marinoni, S.. Osservatorio Astronomico di Bologna; ItaliaFil: Vauclair, G.. Université Paul Sabatier; FranciaFil: Dolez, N.. Université Paul Sabatier; FranciaFil: Chevreton, M.. Observatoire de Paris-Meudon; FranciaFil: Dreizler, S.. Institut für Astrophysik; AlemaniaFil: Schuh, S.. Institut für Astrophysik; AlemaniaFil: Deetjen, J.. Institut für Astrophysik; AlemaniaFil: Nagel, T.. Institut für Astrophysik; AlemaniaFil: Solheim, J.-E.. Universitetet i Tromsø; NoruegaFil: González Pérez, J. M.. Universitetet i Tromsø; NoruegaFil: 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; 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; ArgentinaEDP Sciences2008-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/44898Costa, J. E. S.; Kepler, S. O.; Winget, D. E.; O'Brien, M. S.; Kawaler, S. D.; et al.; The pulsation modes of the pre-white dwarf PG 1159-035; EDP Sciences; Astronomy and Astrophysics; 477; 2; 12-2008; 627-6400004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20053470info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2008/02/aa3470-05/aa3470-05.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 Técnicas2025-10-22T11:10:17Zoai:ri.conicet.gov.ar:11336/44898instacron: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:34982025-10-22 11:10:18.207CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The pulsation modes of the pre-white dwarf PG 1159-035
title The pulsation modes of the pre-white dwarf PG 1159-035
spellingShingle The pulsation modes of the pre-white dwarf PG 1159-035
Costa, J. E. S.
Oscillations
PG 1159-035 (estrella)
Interior stars
White dwarfs
title_short The pulsation modes of the pre-white dwarf PG 1159-035
title_full The pulsation modes of the pre-white dwarf PG 1159-035
title_fullStr The pulsation modes of the pre-white dwarf PG 1159-035
title_full_unstemmed The pulsation modes of the pre-white dwarf PG 1159-035
title_sort The pulsation modes of the pre-white dwarf PG 1159-035
dc.creator.none.fl_str_mv Costa, J. E. S.
Kepler, S. O.
Winget, D. E.
O'Brien, M. S.
Kawaler, S. D.
Costa, A. F. M.
Giovannini, O.
Kanaan, A.
Mukadam, A. S.
Mullally, F.
Nitta, A.
Provençal, J. L.
Shipman, H.
Wood, M. A.
Ahrens, T. J.
Grauer, A.
Kilic, M.
Bradley, P. A.
Sekiguchi, K.
Crowe, R.
Jiang, X. J.
Sullivan, D.
Sullivan, T.
Rosen, R.
Clemens, J. C.
Janulis, R.
O'Donoghue, D.
Ogloza, W.
Baran, A.
Silvotti, R.
Marinoni, S.
Vauclair, G.
Dolez, N.
Chevreton, M.
Dreizler, S.
Schuh, S.
Deetjen, J.
Nagel, T.
Solheim, J.-E.
González Pérez, J. M.
Althaus, Leandro Gabriel
Corsico, Alejandro Hugo
author Costa, J. E. S.
author_facet Costa, J. E. S.
Kepler, S. O.
Winget, D. E.
O'Brien, M. S.
Kawaler, S. D.
Costa, A. F. M.
Giovannini, O.
Kanaan, A.
Mukadam, A. S.
Mullally, F.
Nitta, A.
Provençal, J. L.
Shipman, H.
Wood, M. A.
Ahrens, T. J.
Grauer, A.
Kilic, M.
Bradley, P. A.
Sekiguchi, K.
Crowe, R.
Jiang, X. J.
Sullivan, D.
Sullivan, T.
Rosen, R.
Clemens, J. C.
Janulis, R.
O'Donoghue, D.
Ogloza, W.
Baran, A.
Silvotti, R.
Marinoni, S.
Vauclair, G.
Dolez, N.
Chevreton, M.
Dreizler, S.
Schuh, S.
Deetjen, J.
Nagel, T.
Solheim, J.-E.
González Pérez, J. M.
Althaus, Leandro Gabriel
Corsico, Alejandro Hugo
author_role author
author2 Kepler, S. O.
Winget, D. E.
O'Brien, M. S.
Kawaler, S. D.
Costa, A. F. M.
Giovannini, O.
Kanaan, A.
Mukadam, A. S.
Mullally, F.
Nitta, A.
Provençal, J. L.
Shipman, H.
Wood, M. A.
Ahrens, T. J.
Grauer, A.
Kilic, M.
Bradley, P. A.
Sekiguchi, K.
Crowe, R.
Jiang, X. J.
Sullivan, D.
Sullivan, T.
Rosen, R.
Clemens, J. C.
Janulis, R.
O'Donoghue, D.
Ogloza, W.
Baran, A.
Silvotti, R.
Marinoni, S.
Vauclair, G.
Dolez, N.
Chevreton, M.
Dreizler, S.
Schuh, S.
Deetjen, J.
Nagel, T.
Solheim, J.-E.
González Pérez, J. M.
Althaus, Leandro Gabriel
Corsico, Alejandro Hugo
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Oscillations
PG 1159-035 (estrella)
Interior stars
White dwarfs
topic Oscillations
PG 1159-035 (estrella)
Interior stars
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.PG 1159-035, a pre-white dwarf with 140 000 K, is the prototype of both two classes: the PG 1159 spectroscopic class and the DOV pulsating class. Previous studies of PG 1159-035 photometric data obtained with the Whole Earth Telescope (WET) showed a rich frequency spectrum allowing the identification of 122 pulsation modes. Analyzing the periods of pulsation, it is possible to measure the stellar mass, the rotational period and the inclination of the rotation axis, to estimate an upper limit for the magnetic field, and even to obtain information about the inner stratification of the star. Aims.We have three principal aims: to increase the number of detected and identified pulsation modes in PG 1159-035, study trapping of the star's pulsation modes, and to improve or constrain the determination of stellar parameters. Methods.We used all available WET photometric data from 1983, 1985, 1989, 1993 and 2002 to identify the pulsation periods. Results.We identified 76 additional pulsation modes, increasing to 198 the number of known pulsation modes in PG 1159-035, the largest number of modes detected in any star besides the Sun. From the period spacing we estimated a mass = 0.59 ± 0.02 for PG 1159-035, with the uncertainty dominated by the models, not the observation. Deviations in the regular period spacing suggest that some of the pulsation modes are trapped, even though the star is a pre-white dwarf and the gravitational settling is ongoing. The position of the transition zone that causes the mode trapping was calculated at = 0.83 ± 0.05. From the multiplet splitting, we calculated the rotational period Prot = 1.3920 ± 0.0008 days and an upper limit for the magnetic field, G. The total power of the pulsation modes at the stellar surface changed less than 30% for = 1 modes and less than 50% for = 2 modes. We find no evidence of linear combinations between the 198 pulsation mode frequencies. PG 1159-035 models have not significative convection zones, supporting the hypothesis that nonlinearity arises in the convection zones in cooler pulsating white dwarf stars.
Fil: Costa, J. E. S.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Kepler, S. O.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Winget, D. E.. University of Texas at Austin; Estados Unidos
Fil: O'Brien, M. S.. University of Yale; Estados Unidos
Fil: Kawaler, S. D.. Iowa Steate University; Estados Unidos
Fil: Costa, A. F. M.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Giovannini, O.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Kanaan, A.. Universidade Federal de Santa Catarina; Brasil
Fil: Mukadam, A. S.. University of Washington; Estados Unidos
Fil: Mullally, F.. University of Texas at Austin; Estados Unidos
Fil: Nitta, A.. Gemini Observatory; Estados Unidos
Fil: Provençal, J. L.. University of Delaware; Estados Unidos
Fil: Shipman, H.. University of Delaware; Estados Unidos
Fil: Wood, M. A.. Florida Institute of Technology; Estados Unidos
Fil: Ahrens, T. J.. Florida Institute of Technology; Estados Unidos
Fil: Grauer, A.. University of Arkansas at Little Rock; Estados Unidos
Fil: Kilic, M.. Ohio State University; Estados Unidos
Fil: Bradley, P. A.. Los Alamos National Laboratory; Estados Unidos
Fil: Sekiguchi, K.. Subaru National Astronomical Observatory of Japan; Japón
Fil: Crowe, R.. University of Hawaii; Estados Unidos
Fil: Jiang, X. J.. Chinese Academy of Sciences; República de China
Fil: Sullivan, D.. University of Victoria; Nueva Zelanda
Fil: Sullivan, T.. University of Victoria; Nueva Zelanda
Fil: Rosen, R.. University of Victoria; Nueva Zelanda
Fil: Clemens, J. C.. University of North Carolina; Estados Unidos
Fil: Janulis, R.. VU Institute of Theoretical Physics and Astronomy; Lituania
Fil: O'Donoghue, D.. South African Astronomical Observatory; Sudáfrica
Fil: Ogloza, W.. Cracow Pedagogical University; Polonia
Fil: Baran, A.. Cracow Pedagogical University; Polonia
Fil: Silvotti, R.. Osservatorio Astronomico di Capodimonte; Italia
Fil: Marinoni, S.. Osservatorio Astronomico di Bologna; Italia
Fil: Vauclair, G.. Université Paul Sabatier; Francia
Fil: Dolez, N.. Université Paul Sabatier; Francia
Fil: Chevreton, M.. Observatoire de Paris-Meudon; Francia
Fil: Dreizler, S.. Institut für Astrophysik; Alemania
Fil: Schuh, S.. Institut für Astrophysik; Alemania
Fil: Deetjen, J.. Institut für Astrophysik; Alemania
Fil: Nagel, T.. Institut für Astrophysik; Alemania
Fil: Solheim, J.-E.. Universitetet i Tromsø; Noruega
Fil: González Pérez, J. M.. Universitetet i Tromsø; Noruega
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
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
description Context.PG 1159-035, a pre-white dwarf with 140 000 K, is the prototype of both two classes: the PG 1159 spectroscopic class and the DOV pulsating class. Previous studies of PG 1159-035 photometric data obtained with the Whole Earth Telescope (WET) showed a rich frequency spectrum allowing the identification of 122 pulsation modes. Analyzing the periods of pulsation, it is possible to measure the stellar mass, the rotational period and the inclination of the rotation axis, to estimate an upper limit for the magnetic field, and even to obtain information about the inner stratification of the star. Aims.We have three principal aims: to increase the number of detected and identified pulsation modes in PG 1159-035, study trapping of the star's pulsation modes, and to improve or constrain the determination of stellar parameters. Methods.We used all available WET photometric data from 1983, 1985, 1989, 1993 and 2002 to identify the pulsation periods. Results.We identified 76 additional pulsation modes, increasing to 198 the number of known pulsation modes in PG 1159-035, the largest number of modes detected in any star besides the Sun. From the period spacing we estimated a mass = 0.59 ± 0.02 for PG 1159-035, with the uncertainty dominated by the models, not the observation. Deviations in the regular period spacing suggest that some of the pulsation modes are trapped, even though the star is a pre-white dwarf and the gravitational settling is ongoing. The position of the transition zone that causes the mode trapping was calculated at = 0.83 ± 0.05. From the multiplet splitting, we calculated the rotational period Prot = 1.3920 ± 0.0008 days and an upper limit for the magnetic field, G. The total power of the pulsation modes at the stellar surface changed less than 30% for = 1 modes and less than 50% for = 2 modes. We find no evidence of linear combinations between the 198 pulsation mode frequencies. PG 1159-035 models have not significative convection zones, supporting the hypothesis that nonlinearity arises in the convection zones in cooler pulsating white dwarf stars.
publishDate 2008
dc.date.none.fl_str_mv 2008-12
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
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://hdl.handle.net/11336/44898
Costa, J. E. S.; Kepler, S. O.; Winget, D. E.; O'Brien, M. S.; Kawaler, S. D.; et al.; The pulsation modes of the pre-white dwarf PG 1159-035; EDP Sciences; Astronomy and Astrophysics; 477; 2; 12-2008; 627-640
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/44898
identifier_str_mv Costa, J. E. S.; Kepler, S. O.; Winget, D. E.; O'Brien, M. S.; Kawaler, S. D.; et al.; The pulsation modes of the pre-white dwarf PG 1159-035; EDP Sciences; Astronomy and Astrophysics; 477; 2; 12-2008; 627-640
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20053470
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2008/02/aa3470-05/aa3470-05.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
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instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 12.982451

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