Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf

Autores
Caliskan, Ozcan; Uzundag, Murat; Kilic, Mukremin; de Gerónimo, Francisco César; Moss, Adam; Corsico, Alejandro Hugo; Parsons, Steven G.; Pelisoli, Ingrid; Jewett, Gracyn; Rebassa-Mansergas, Alberto; Brown, Alex J.; Dhillon, Vikram S.; Bergeron, Pierre
Año de publicación
2025
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present extensive follow-up time-series photometry of WD J0049‑2525, the most massive pulsating white dwarf currently known, with Teff = 13,020 K and logg=9.34 cm s‑2. The discovery observations detected only two significant pulsation modes. Here, we report the detection of 13 significant pulsation modes ranging from 170 to 258 s based on 11 nights of observations with the New Technology Telescope, Gemini, and Apache Point Observatory telescopes. We use these 13 modes to perform asteroseismology and find that the best-fitting models (under the assumption of an ONe core composition) have M⋆ ≈ 1.29M⊙, a surface hydrogen layer mass of log(MH/M⋆)≲‑7.5 , and a crystallized core fraction of >99%. An analysis of the period spacing also strongly suggests a very high mass. The asteroseismic distance derived is in good agreement with the distance provided by Gaia. We also find tentative evidence of a rotation period of 0.3 or 0.67 days. This analysis provides the first look at the interior of a ∼1.3 M⊙ white dwarf.
Fil: Caliskan, Ozcan. Oklahoma State University; Estados Unidos
Fil: Uzundag, Murat. Institute of Astronomy; Bélgica
Fil: Kilic, Mukremin. Oklahoma State University; Estados Unidos
Fil: de Gerónimo, Francisco César. 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: Moss, Adam. Oklahoma State University; Estados Unidos
Fil: Corsico, Alejandro Hugo. 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: Parsons, Steven G.. University of Sheffield;
Fil: Pelisoli, Ingrid. University of Warwick; Reino Unido
Fil: Jewett, Gracyn. Oklahoma State University; Estados Unidos
Fil: Rebassa-Mansergas, Alberto. Universidad Politécnica de Catalunya; España
Fil: Brown, Alex J.. Universitat Hamburg; Alemania
Fil: Dhillon, Vikram S.. University of Sheffield;
Fil: Bergeron, Pierre. University of Montreal; Canadá
Materia
WHITE DWARFS
ASTEROSEISMOLOGY
PULSATION MODES
ZZ CETI
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/290716
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/290716
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White DwarfCaliskan, OzcanUzundag, MuratKilic, Mukreminde Gerónimo, Francisco CésarMoss, AdamCorsico, Alejandro HugoParsons, Steven G.Pelisoli, IngridJewett, GracynRebassa-Mansergas, AlbertoBrown, Alex J.Dhillon, Vikram S.Bergeron, PierreWHITE DWARFSASTEROSEISMOLOGYPULSATION MODESZZ CETIhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present extensive follow-up time-series photometry of WD J0049‑2525, the most massive pulsating white dwarf currently known, with Teff = 13,020 K and logg=9.34 cm s‑2. The discovery observations detected only two significant pulsation modes. Here, we report the detection of 13 significant pulsation modes ranging from 170 to 258 s based on 11 nights of observations with the New Technology Telescope, Gemini, and Apache Point Observatory telescopes. We use these 13 modes to perform asteroseismology and find that the best-fitting models (under the assumption of an ONe core composition) have M⋆ ≈ 1.29M⊙, a surface hydrogen layer mass of log(MH/M⋆)≲‑7.5 , and a crystallized core fraction of >99%. An analysis of the period spacing also strongly suggests a very high mass. The asteroseismic distance derived is in good agreement with the distance provided by Gaia. We also find tentative evidence of a rotation period of 0.3 or 0.67 days. This analysis provides the first look at the interior of a ∼1.3 M⊙ white dwarf.Fil: Caliskan, Ozcan. Oklahoma State University; Estados UnidosFil: Uzundag, Murat. Institute of Astronomy; BélgicaFil: Kilic, Mukremin. Oklahoma State University; Estados UnidosFil: de Gerónimo, Francisco César. 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: Moss, Adam. Oklahoma State University; Estados UnidosFil: Corsico, Alejandro Hugo. 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: Parsons, Steven G.. University of Sheffield;Fil: Pelisoli, Ingrid. University of Warwick; Reino UnidoFil: Jewett, Gracyn. Oklahoma State University; Estados UnidosFil: Rebassa-Mansergas, Alberto. Universidad Politécnica de Catalunya; EspañaFil: Brown, Alex J.. Universitat Hamburg; AlemaniaFil: Dhillon, Vikram S.. University of Sheffield;Fil: Bergeron, Pierre. University of Montreal; CanadáIOP Publishing2025-07info: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/11336/290716Caliskan, Ozcan; Uzundag, Murat; Kilic, Mukremin; de Gerónimo, Francisco César; Moss, Adam; et al.; Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf; IOP Publishing; Astrophysical Journal; 988; 1; 7-2025; 1-110004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/addc70info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/addc70info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2026-08-25T14:34:30Zoai:ri.conicet.gov.ar:11336/290716instacron: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:34982026-08-25 14:34:30.615CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf
title Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf
spellingShingle Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf
Caliskan, Ozcan
WHITE DWARFS
ASTEROSEISMOLOGY
PULSATION MODES
ZZ CETI
title_short Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf
title_full Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf
title_fullStr Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf
title_full_unstemmed Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf
title_sort Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf
dc.creator.none.fl_str_mv Caliskan, Ozcan
Uzundag, Murat
Kilic, Mukremin
de Gerónimo, Francisco César
Moss, Adam
Corsico, Alejandro Hugo
Parsons, Steven G.
Pelisoli, Ingrid
Jewett, Gracyn
Rebassa-Mansergas, Alberto
Brown, Alex J.
Dhillon, Vikram S.
Bergeron, Pierre
author Caliskan, Ozcan
author_facet Caliskan, Ozcan
Uzundag, Murat
Kilic, Mukremin
de Gerónimo, Francisco César
Moss, Adam
Corsico, Alejandro Hugo
Parsons, Steven G.
Pelisoli, Ingrid
Jewett, Gracyn
Rebassa-Mansergas, Alberto
Brown, Alex J.
Dhillon, Vikram S.
Bergeron, Pierre
author_role author
author2 Uzundag, Murat
Kilic, Mukremin
de Gerónimo, Francisco César
Moss, Adam
Corsico, Alejandro Hugo
Parsons, Steven G.
Pelisoli, Ingrid
Jewett, Gracyn
Rebassa-Mansergas, Alberto
Brown, Alex J.
Dhillon, Vikram S.
Bergeron, Pierre
author2_role author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv WHITE DWARFS
ASTEROSEISMOLOGY
PULSATION MODES
ZZ CETI
topic WHITE DWARFS
ASTEROSEISMOLOGY
PULSATION MODES
ZZ CETI
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We present extensive follow-up time-series photometry of WD J0049‑2525, the most massive pulsating white dwarf currently known, with Teff = 13,020 K and logg=9.34 cm s‑2. The discovery observations detected only two significant pulsation modes. Here, we report the detection of 13 significant pulsation modes ranging from 170 to 258 s based on 11 nights of observations with the New Technology Telescope, Gemini, and Apache Point Observatory telescopes. We use these 13 modes to perform asteroseismology and find that the best-fitting models (under the assumption of an ONe core composition) have M⋆ ≈ 1.29M⊙, a surface hydrogen layer mass of log(MH/M⋆)≲‑7.5 , and a crystallized core fraction of >99%. An analysis of the period spacing also strongly suggests a very high mass. The asteroseismic distance derived is in good agreement with the distance provided by Gaia. We also find tentative evidence of a rotation period of 0.3 or 0.67 days. This analysis provides the first look at the interior of a ∼1.3 M⊙ white dwarf.
Fil: Caliskan, Ozcan. Oklahoma State University; Estados Unidos
Fil: Uzundag, Murat. Institute of Astronomy; Bélgica
Fil: Kilic, Mukremin. Oklahoma State University; Estados Unidos
Fil: de Gerónimo, Francisco César. 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: Moss, Adam. Oklahoma State University; Estados Unidos
Fil: Corsico, Alejandro Hugo. 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: Parsons, Steven G.. University of Sheffield;
Fil: Pelisoli, Ingrid. University of Warwick; Reino Unido
Fil: Jewett, Gracyn. Oklahoma State University; Estados Unidos
Fil: Rebassa-Mansergas, Alberto. Universidad Politécnica de Catalunya; España
Fil: Brown, Alex J.. Universitat Hamburg; Alemania
Fil: Dhillon, Vikram S.. University of Sheffield;
Fil: Bergeron, Pierre. University of Montreal; Canadá
description We present extensive follow-up time-series photometry of WD J0049‑2525, the most massive pulsating white dwarf currently known, with Teff = 13,020 K and logg=9.34 cm s‑2. The discovery observations detected only two significant pulsation modes. Here, we report the detection of 13 significant pulsation modes ranging from 170 to 258 s based on 11 nights of observations with the New Technology Telescope, Gemini, and Apache Point Observatory telescopes. We use these 13 modes to perform asteroseismology and find that the best-fitting models (under the assumption of an ONe core composition) have M⋆ ≈ 1.29M⊙, a surface hydrogen layer mass of log(MH/M⋆)≲‑7.5 , and a crystallized core fraction of >99%. An analysis of the period spacing also strongly suggests a very high mass. The asteroseismic distance derived is in good agreement with the distance provided by Gaia. We also find tentative evidence of a rotation period of 0.3 or 0.67 days. This analysis provides the first look at the interior of a ∼1.3 M⊙ white dwarf.
publishDate 2025
dc.date.none.fl_str_mv 2025-07
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/11336/290716
Caliskan, Ozcan; Uzundag, Murat; Kilic, Mukremin; de Gerónimo, Francisco César; Moss, Adam; et al.; Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf; IOP Publishing; Astrophysical Journal; 988; 1; 7-2025; 1-11
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/290716
identifier_str_mv Caliskan, Ozcan; Uzundag, Murat; Kilic, Mukremin; de Gerónimo, Francisco César; Moss, Adam; et al.; Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf; IOP Publishing; Astrophysical Journal; 988; 1; 7-2025; 1-11
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/addc70
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/addc70
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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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score 13.265058

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