The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200

Autores
Vauclair, G.; Fu, J. N.; Solheim, J. E.; Kim, S. l.; Dolez, N.; Chevreton, M.; Chen, L.; Wood, M. A.; Silver, I. M.; Bognár, Z.; Paparó, M.; Corsico, Alejandro Hugo
Año de publicación
2011
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. The PG 1159 pre-white dwarf stars experiment a rapidly cooling phase with a time scale of a few 106 years. Theoretical models predict that the neutrinos produced in their core should play a dominant role in the cooling, mainly at the cool end of the PG 1159 sequence. Measuring the evolutionary time scale of the coolest PG 1159 stars could offer a unique opportunity to empirically constrain the neutrino emission rate. Aims. A subgroup of the PG 1159 stars are nonradial pulsators, the GW Vir type of variable stars. They exhibit g-mode pulsations with periods of a few hundred seconds. As the stars cool, the pulsation frequencies evolve according to the change in their internal structure. It was anticipated that the measurement of their rate of change would directly determine the evolution time scale and so constrain the neutrino emission rates. As PG 0122+200 (BB Psc) defines the red edge of the GW Vir instability strip, it is a good candidate for such a measurement. Methods. The pulsations of PG 0122+200 have been observed during 22 years from 1986 to 2008, through the fast photometry technique. We used those data to measure the rate of change of its frequencies and amplitudes. Results. Among the 24 identified ℓ = 1 modes, the frequency and amplitude variations have been obtained for the seven largest amplitude ones. We find changes of their frequency of much larger amplitudes and shorter time scales than the one predicted by theoretical models that assume that the cooling dominates the frequency variations. In the case of the largest amplitude mode at 2497 μHz (400 s), its variations are best fitted by a combination of two terms: one long term with a time scale of 5.4 × 104 years, which is significantly shorter than the predicted evolutionary time scale of 8 × 106 years; and one additional periodic term with a period of either 261 or 211 days. Some other mechanism(s) than the cooling must be responsible for such variations. We suggest that the resonant coupling induced within triplets by the star rotation could be such a mechanism. As a consequence, no useful constraints on the neutrino emission rate can presently be derived as long as the dominant mechanism is not properly understood. Conclusions. The temporal variations in the pulsation frequencies observed in PG 0122+200 cannot be simply attributed to the cooling of the star, regardless of the contribution of the neutrino losses. Our results suggest that the resonant coupling induced by the rotation plays a dominant role which must be further investigated.
Fil: Vauclair, G.. Centre National de la Recherche Scientifique; Francia
Fil: Fu, J. N.. Beijing Normal University. Department of Astronomy; China
Fil: Solheim, J. E.. University of Oslo. Institute of Theoretical Astrophysics; Noruega
Fil: Kim, S. l. . Korea Astronomy and Space Science Institute; Corea del Sur
Fil: Dolez, N.. Centre National de la Recherche Scientifique; Francia
Fil: Chevreton, M.. Observatoire de Paris-Meudon; Francia
Fil: Chen, L.. Beijing Normal University. Department of Astronomy; China
Fil: Wood, M. A. . Florida Institute of Technology. Department of Physics and Space Sciences & SARA Observatory; Estados Unidos
Fil: Silver, I. M. . Florida Institute of Technology. Department of Physics and Space Sciences & SARA Observatory; Estados Unidos
Fil: Bognár, Z.. Konkoly Observatory; Hungría
Fil: Paparó, M.. Konkoly Observatory; Hungría
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 La Plata. Instituto de Astrofísica de La Plata; Argentina
Materia
Evolution of stars
White dwarfs
PG 0122+200 (estrella)
Star pulsations
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:11336/10109

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network_acronym_str CONICETDig
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network_name_str CONICET Digital (CONICET)
spelling The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200Vauclair, G.Fu, J. N.Solheim, J. E.Kim, S. l. Dolez, N.Chevreton, M.Chen, L.Wood, M. A. Silver, I. M. Bognár, Z.Paparó, M.Corsico, Alejandro HugoEvolution of starsWhite dwarfsPG 0122+200 (estrella)Star pulsationshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The PG 1159 pre-white dwarf stars experiment a rapidly cooling phase with a time scale of a few 106 years. Theoretical models predict that the neutrinos produced in their core should play a dominant role in the cooling, mainly at the cool end of the PG 1159 sequence. Measuring the evolutionary time scale of the coolest PG 1159 stars could offer a unique opportunity to empirically constrain the neutrino emission rate. Aims. A subgroup of the PG 1159 stars are nonradial pulsators, the GW Vir type of variable stars. They exhibit g-mode pulsations with periods of a few hundred seconds. As the stars cool, the pulsation frequencies evolve according to the change in their internal structure. It was anticipated that the measurement of their rate of change would directly determine the evolution time scale and so constrain the neutrino emission rates. As PG 0122+200 (BB Psc) defines the red edge of the GW Vir instability strip, it is a good candidate for such a measurement. Methods. The pulsations of PG 0122+200 have been observed during 22 years from 1986 to 2008, through the fast photometry technique. We used those data to measure the rate of change of its frequencies and amplitudes. Results. Among the 24 identified ℓ = 1 modes, the frequency and amplitude variations have been obtained for the seven largest amplitude ones. We find changes of their frequency of much larger amplitudes and shorter time scales than the one predicted by theoretical models that assume that the cooling dominates the frequency variations. In the case of the largest amplitude mode at 2497 μHz (400 s), its variations are best fitted by a combination of two terms: one long term with a time scale of 5.4 × 104 years, which is significantly shorter than the predicted evolutionary time scale of 8 × 106 years; and one additional periodic term with a period of either 261 or 211 days. Some other mechanism(s) than the cooling must be responsible for such variations. We suggest that the resonant coupling induced within triplets by the star rotation could be such a mechanism. As a consequence, no useful constraints on the neutrino emission rate can presently be derived as long as the dominant mechanism is not properly understood. Conclusions. The temporal variations in the pulsation frequencies observed in PG 0122+200 cannot be simply attributed to the cooling of the star, regardless of the contribution of the neutrino losses. Our results suggest that the resonant coupling induced by the rotation plays a dominant role which must be further investigated.Fil: Vauclair, G.. Centre National de la Recherche Scientifique; FranciaFil: Fu, J. N.. Beijing Normal University. Department of Astronomy; ChinaFil: Solheim, J. E.. University of Oslo. Institute of Theoretical Astrophysics; NoruegaFil: Kim, S. l. . Korea Astronomy and Space Science Institute; Corea del SurFil: Dolez, N.. Centre National de la Recherche Scientifique; FranciaFil: Chevreton, M.. Observatoire de Paris-Meudon; FranciaFil: Chen, L.. Beijing Normal University. Department of Astronomy; ChinaFil: Wood, M. A. . Florida Institute of Technology. Department of Physics and Space Sciences & SARA Observatory; Estados UnidosFil: Silver, I. M. . Florida Institute of Technology. Department of Physics and Space Sciences & SARA Observatory; Estados UnidosFil: Bognár, Z.. Konkoly Observatory; HungríaFil: Paparó, M.. Konkoly Observatory; HungríaFil: 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 La Plata. Instituto de Astrofísica de La Plata; ArgentinaEdp Sciences2011-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/10109Vauclair, G.; Fu, J. N.; Solheim, J. E.; Kim, S. l. ; Dolez, N.; et al.; The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200; Edp Sciences; Astronomy And Astrophysics; 528; 4-2011; 5-150004-6361enginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201014457info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2011/04/aa14457-10/aa14457-10.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 Técnicas2025-09-29T10:33:07Zoai:ri.conicet.gov.ar:11336/10109instacron: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 10:33:07.994CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200
title The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200
spellingShingle The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200
Vauclair, G.
Evolution of stars
White dwarfs
PG 0122+200 (estrella)
Star pulsations
title_short The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200
title_full The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200
title_fullStr The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200
title_full_unstemmed The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200
title_sort The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200
dc.creator.none.fl_str_mv Vauclair, G.
Fu, J. N.
Solheim, J. E.
Kim, S. l.
Dolez, N.
Chevreton, M.
Chen, L.
Wood, M. A.
Silver, I. M.
Bognár, Z.
Paparó, M.
Corsico, Alejandro Hugo
author Vauclair, G.
author_facet Vauclair, G.
Fu, J. N.
Solheim, J. E.
Kim, S. l.
Dolez, N.
Chevreton, M.
Chen, L.
Wood, M. A.
Silver, I. M.
Bognár, Z.
Paparó, M.
Corsico, Alejandro Hugo
author_role author
author2 Fu, J. N.
Solheim, J. E.
Kim, S. l.
Dolez, N.
Chevreton, M.
Chen, L.
Wood, M. A.
Silver, I. M.
Bognár, Z.
Paparó, M.
Corsico, Alejandro Hugo
author2_role author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Evolution of stars
White dwarfs
PG 0122+200 (estrella)
Star pulsations
topic Evolution of stars
White dwarfs
PG 0122+200 (estrella)
Star pulsations
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. The PG 1159 pre-white dwarf stars experiment a rapidly cooling phase with a time scale of a few 106 years. Theoretical models predict that the neutrinos produced in their core should play a dominant role in the cooling, mainly at the cool end of the PG 1159 sequence. Measuring the evolutionary time scale of the coolest PG 1159 stars could offer a unique opportunity to empirically constrain the neutrino emission rate. Aims. A subgroup of the PG 1159 stars are nonradial pulsators, the GW Vir type of variable stars. They exhibit g-mode pulsations with periods of a few hundred seconds. As the stars cool, the pulsation frequencies evolve according to the change in their internal structure. It was anticipated that the measurement of their rate of change would directly determine the evolution time scale and so constrain the neutrino emission rates. As PG 0122+200 (BB Psc) defines the red edge of the GW Vir instability strip, it is a good candidate for such a measurement. Methods. The pulsations of PG 0122+200 have been observed during 22 years from 1986 to 2008, through the fast photometry technique. We used those data to measure the rate of change of its frequencies and amplitudes. Results. Among the 24 identified ℓ = 1 modes, the frequency and amplitude variations have been obtained for the seven largest amplitude ones. We find changes of their frequency of much larger amplitudes and shorter time scales than the one predicted by theoretical models that assume that the cooling dominates the frequency variations. In the case of the largest amplitude mode at 2497 μHz (400 s), its variations are best fitted by a combination of two terms: one long term with a time scale of 5.4 × 104 years, which is significantly shorter than the predicted evolutionary time scale of 8 × 106 years; and one additional periodic term with a period of either 261 or 211 days. Some other mechanism(s) than the cooling must be responsible for such variations. We suggest that the resonant coupling induced within triplets by the star rotation could be such a mechanism. As a consequence, no useful constraints on the neutrino emission rate can presently be derived as long as the dominant mechanism is not properly understood. Conclusions. The temporal variations in the pulsation frequencies observed in PG 0122+200 cannot be simply attributed to the cooling of the star, regardless of the contribution of the neutrino losses. Our results suggest that the resonant coupling induced by the rotation plays a dominant role which must be further investigated.
Fil: Vauclair, G.. Centre National de la Recherche Scientifique; Francia
Fil: Fu, J. N.. Beijing Normal University. Department of Astronomy; China
Fil: Solheim, J. E.. University of Oslo. Institute of Theoretical Astrophysics; Noruega
Fil: Kim, S. l. . Korea Astronomy and Space Science Institute; Corea del Sur
Fil: Dolez, N.. Centre National de la Recherche Scientifique; Francia
Fil: Chevreton, M.. Observatoire de Paris-Meudon; Francia
Fil: Chen, L.. Beijing Normal University. Department of Astronomy; China
Fil: Wood, M. A. . Florida Institute of Technology. Department of Physics and Space Sciences & SARA Observatory; Estados Unidos
Fil: Silver, I. M. . Florida Institute of Technology. Department of Physics and Space Sciences & SARA Observatory; Estados Unidos
Fil: Bognár, Z.. Konkoly Observatory; Hungría
Fil: Paparó, M.. Konkoly Observatory; Hungría
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 La Plata. Instituto de Astrofísica de La Plata; Argentina
description Context. The PG 1159 pre-white dwarf stars experiment a rapidly cooling phase with a time scale of a few 106 years. Theoretical models predict that the neutrinos produced in their core should play a dominant role in the cooling, mainly at the cool end of the PG 1159 sequence. Measuring the evolutionary time scale of the coolest PG 1159 stars could offer a unique opportunity to empirically constrain the neutrino emission rate. Aims. A subgroup of the PG 1159 stars are nonradial pulsators, the GW Vir type of variable stars. They exhibit g-mode pulsations with periods of a few hundred seconds. As the stars cool, the pulsation frequencies evolve according to the change in their internal structure. It was anticipated that the measurement of their rate of change would directly determine the evolution time scale and so constrain the neutrino emission rates. As PG 0122+200 (BB Psc) defines the red edge of the GW Vir instability strip, it is a good candidate for such a measurement. Methods. The pulsations of PG 0122+200 have been observed during 22 years from 1986 to 2008, through the fast photometry technique. We used those data to measure the rate of change of its frequencies and amplitudes. Results. Among the 24 identified ℓ = 1 modes, the frequency and amplitude variations have been obtained for the seven largest amplitude ones. We find changes of their frequency of much larger amplitudes and shorter time scales than the one predicted by theoretical models that assume that the cooling dominates the frequency variations. In the case of the largest amplitude mode at 2497 μHz (400 s), its variations are best fitted by a combination of two terms: one long term with a time scale of 5.4 × 104 years, which is significantly shorter than the predicted evolutionary time scale of 8 × 106 years; and one additional periodic term with a period of either 261 or 211 days. Some other mechanism(s) than the cooling must be responsible for such variations. We suggest that the resonant coupling induced within triplets by the star rotation could be such a mechanism. As a consequence, no useful constraints on the neutrino emission rate can presently be derived as long as the dominant mechanism is not properly understood. Conclusions. The temporal variations in the pulsation frequencies observed in PG 0122+200 cannot be simply attributed to the cooling of the star, regardless of the contribution of the neutrino losses. Our results suggest that the resonant coupling induced by the rotation plays a dominant role which must be further investigated.
publishDate 2011
dc.date.none.fl_str_mv 2011-04
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/11336/10109
Vauclair, G.; Fu, J. N.; Solheim, J. E.; Kim, S. l. ; Dolez, N.; et al.; The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200; Edp Sciences; Astronomy And Astrophysics; 528; 4-2011; 5-15
0004-6361
url http://hdl.handle.net/11336/10109
identifier_str_mv Vauclair, G.; Fu, J. N.; Solheim, J. E.; Kim, S. l. ; Dolez, N.; et al.; The period and amplitude changes in the coolest GW Virginis variable star (PG 1159-type) PG 0122+200; Edp Sciences; Astronomy And Astrophysics; 528; 4-2011; 5-15
0004-6361
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201014457
info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2011/04/aa14457-10/aa14457-10.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
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)
collection CONICET Digital (CONICET)
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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