Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093
- Autores
- Nitta, Atsuko; Kepler, S. O.; Chené, André Nicolás; Koester, D.; Provencal, J. L.; Kleinmani, S. J.; Sullivan, D. J.; Chote, Paul; Sefako, Ramotholo; Kanann, Antonio; Romero, Alejandra D.; Corti, Mariela Alejandra; Kilic, Mukremin; Montgomery, M. H.; Winget, D.
- Año de publicación
- 2016
- Idioma
- inglés
- Tipo de recurso
- documento de conferencia
- Estado
- versión publicada
- Descripción
- We are trying to reduce the largest uncertainties in using white dwarf stars as Galactic chronometers by understanding the details of carbon crystalliazation that currently result in a 1–2 Gyr uncertainty in the ages of the oldest white dwarf stars. We expect the coolest white dwarf stars to have crystallized interiors, but theory also predicts hotter white dwarf stars, if they are massive enough, will also have some core crystallization. BPM 37093 is the first discovered of only a handful of known massive white dwarf stars that are also pulsating DAV, or ZZ Ceti, variables. Our approach is to use the pulsations to constrain the core composition and amount of crystallization. Here we report our analysis of 4 hours of continuous time series spectroscopy of BPM 37093 with Gemini South combined with simultaneous time-series photometry from Mt. John (New Zealand), SAAO, PROMPT, and Complejo Astronomico El Leoncito (CASLEO, Argentina).
Fil: Nitta, Atsuko. Gemini Observatory; Estados Unidos
Fil: Kepler, S. O.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Chené, André Nicolás. Gemini Observatory; Estados Unidos
Fil: Koester, D.. Universitat Kiel; Alemania
Fil: Provencal, J. L.. University of Delaware; Estados Unidos
Fil: Kleinmani, S. J.. Gemini Observatory; Estados Unidos
Fil: Sullivan, D. J.. Victoria University of Wellington; Nueva Zelanda
Fil: Chote, Paul. University of Warwick; Reino Unido
Fil: Sefako, Ramotholo. South African Astronomical Observatory; Sudáfrica
Fil: Kanann, Antonio. Universidade Federal de Santa Catarina; Brasil
Fil: Romero, Alejandra D.. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Corti, Mariela Alejandra. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Kilic, Mukremin. University of Oklahoma; Estados Unidos
Fil: Montgomery, M. H.. University of Texas at Austin; Estados Unidos
Fil: Winget, D.. University of Texas at Austin; Estados Unidos
XXIX IAU General Assembly
Honolulu
Estados Unidos
International Astronomical Union - Materia
-
STARS:WHITE DWARFS
STARS:VARIABLES:OTHERS
STARS:EVOLUTION - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/138961
Ver los metadatos del registro completo
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Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093Nitta, AtsukoKepler, S. O.Chené, André NicolásKoester, D.Provencal, J. L.Kleinmani, S. J.Sullivan, D. J.Chote, PaulSefako, RamotholoKanann, AntonioRomero, Alejandra D.Corti, Mariela AlejandraKilic, MukreminMontgomery, M. H.Winget, D.STARS:WHITE DWARFSSTARS:VARIABLES:OTHERSSTARS:EVOLUTIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We are trying to reduce the largest uncertainties in using white dwarf stars as Galactic chronometers by understanding the details of carbon crystalliazation that currently result in a 1–2 Gyr uncertainty in the ages of the oldest white dwarf stars. We expect the coolest white dwarf stars to have crystallized interiors, but theory also predicts hotter white dwarf stars, if they are massive enough, will also have some core crystallization. BPM 37093 is the first discovered of only a handful of known massive white dwarf stars that are also pulsating DAV, or ZZ Ceti, variables. Our approach is to use the pulsations to constrain the core composition and amount of crystallization. Here we report our analysis of 4 hours of continuous time series spectroscopy of BPM 37093 with Gemini South combined with simultaneous time-series photometry from Mt. John (New Zealand), SAAO, PROMPT, and Complejo Astronomico El Leoncito (CASLEO, Argentina).Fil: Nitta, Atsuko. Gemini Observatory; Estados UnidosFil: Kepler, S. O.. Universidade Federal do Rio Grande do Sul; BrasilFil: Chené, André Nicolás. Gemini Observatory; Estados UnidosFil: Koester, D.. Universitat Kiel; AlemaniaFil: Provencal, J. L.. University of Delaware; Estados UnidosFil: Kleinmani, S. J.. Gemini Observatory; Estados UnidosFil: Sullivan, D. J.. Victoria University of Wellington; Nueva ZelandaFil: Chote, Paul. University of Warwick; Reino UnidoFil: Sefako, Ramotholo. South African Astronomical Observatory; SudáfricaFil: Kanann, Antonio. Universidade Federal de Santa Catarina; BrasilFil: Romero, Alejandra D.. Universidade Federal do Rio Grande do Sul; BrasilFil: Corti, Mariela Alejandra. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Kilic, Mukremin. University of Oklahoma; Estados UnidosFil: Montgomery, M. H.. University of Texas at Austin; Estados UnidosFil: Winget, D.. University of Texas at Austin; Estados UnidosXXIX IAU General AssemblyHonoluluEstados UnidosInternational Astronomical UnionCambridge University PressStorchi Bergmann, ThaisaForman, WilliamOverzier, RoderikRiffel, Rogério2016info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/conferenceObjectConferenciaJournalhttp://purl.org/coar/resource_type/c_5794info:ar-repo/semantics/documentoDeConferenciaapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/138961Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093; XXIX IAU General Assembly; Honolulu; Estados Unidos; 2015; 493-4961743-92131743-9221CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1017/S1743921316005962info:eu-repo/semantics/altIdentifier/url/https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/constraining-the-physics-of-carbon-crystallization-through-pulsations-of-a-massive-dav-bpm37093/8D9F75390F58BA99E8BF8D6967B0202DInternacionalinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:34:47Zoai:ri.conicet.gov.ar:11336/138961instacron: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 10:34:47.514CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093 |
| title |
Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093 |
| spellingShingle |
Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093 Nitta, Atsuko STARS:WHITE DWARFS STARS:VARIABLES:OTHERS STARS:EVOLUTION |
| title_short |
Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093 |
| title_full |
Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093 |
| title_fullStr |
Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093 |
| title_full_unstemmed |
Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093 |
| title_sort |
Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093 |
| dc.creator.none.fl_str_mv |
Nitta, Atsuko Kepler, S. O. Chené, André Nicolás Koester, D. Provencal, J. L. Kleinmani, S. J. Sullivan, D. J. Chote, Paul Sefako, Ramotholo Kanann, Antonio Romero, Alejandra D. Corti, Mariela Alejandra Kilic, Mukremin Montgomery, M. H. Winget, D. |
| author |
Nitta, Atsuko |
| author_facet |
Nitta, Atsuko Kepler, S. O. Chené, André Nicolás Koester, D. Provencal, J. L. Kleinmani, S. J. Sullivan, D. J. Chote, Paul Sefako, Ramotholo Kanann, Antonio Romero, Alejandra D. Corti, Mariela Alejandra Kilic, Mukremin Montgomery, M. H. Winget, D. |
| author_role |
author |
| author2 |
Kepler, S. O. Chené, André Nicolás Koester, D. Provencal, J. L. Kleinmani, S. J. Sullivan, D. J. Chote, Paul Sefako, Ramotholo Kanann, Antonio Romero, Alejandra D. Corti, Mariela Alejandra Kilic, Mukremin Montgomery, M. H. Winget, D. |
| author2_role |
author author author author author author author author author author author author author author |
| dc.contributor.none.fl_str_mv |
Storchi Bergmann, Thaisa Forman, William Overzier, Roderik Riffel, Rogério |
| dc.subject.none.fl_str_mv |
STARS:WHITE DWARFS STARS:VARIABLES:OTHERS STARS:EVOLUTION |
| topic |
STARS:WHITE DWARFS STARS:VARIABLES:OTHERS STARS:EVOLUTION |
| 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 are trying to reduce the largest uncertainties in using white dwarf stars as Galactic chronometers by understanding the details of carbon crystalliazation that currently result in a 1–2 Gyr uncertainty in the ages of the oldest white dwarf stars. We expect the coolest white dwarf stars to have crystallized interiors, but theory also predicts hotter white dwarf stars, if they are massive enough, will also have some core crystallization. BPM 37093 is the first discovered of only a handful of known massive white dwarf stars that are also pulsating DAV, or ZZ Ceti, variables. Our approach is to use the pulsations to constrain the core composition and amount of crystallization. Here we report our analysis of 4 hours of continuous time series spectroscopy of BPM 37093 with Gemini South combined with simultaneous time-series photometry from Mt. John (New Zealand), SAAO, PROMPT, and Complejo Astronomico El Leoncito (CASLEO, Argentina). Fil: Nitta, Atsuko. Gemini Observatory; Estados Unidos Fil: Kepler, S. O.. Universidade Federal do Rio Grande do Sul; Brasil Fil: Chené, André Nicolás. Gemini Observatory; Estados Unidos Fil: Koester, D.. Universitat Kiel; Alemania Fil: Provencal, J. L.. University of Delaware; Estados Unidos Fil: Kleinmani, S. J.. Gemini Observatory; Estados Unidos Fil: Sullivan, D. J.. Victoria University of Wellington; Nueva Zelanda Fil: Chote, Paul. University of Warwick; Reino Unido Fil: Sefako, Ramotholo. South African Astronomical Observatory; Sudáfrica Fil: Kanann, Antonio. Universidade Federal de Santa Catarina; Brasil Fil: Romero, Alejandra D.. Universidade Federal do Rio Grande do Sul; Brasil Fil: Corti, Mariela Alejandra. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina Fil: Kilic, Mukremin. University of Oklahoma; Estados Unidos Fil: Montgomery, M. H.. University of Texas at Austin; Estados Unidos Fil: Winget, D.. University of Texas at Austin; Estados Unidos XXIX IAU General Assembly Honolulu Estados Unidos International Astronomical Union |
| description |
We are trying to reduce the largest uncertainties in using white dwarf stars as Galactic chronometers by understanding the details of carbon crystalliazation that currently result in a 1–2 Gyr uncertainty in the ages of the oldest white dwarf stars. We expect the coolest white dwarf stars to have crystallized interiors, but theory also predicts hotter white dwarf stars, if they are massive enough, will also have some core crystallization. BPM 37093 is the first discovered of only a handful of known massive white dwarf stars that are also pulsating DAV, or ZZ Ceti, variables. Our approach is to use the pulsations to constrain the core composition and amount of crystallization. Here we report our analysis of 4 hours of continuous time series spectroscopy of BPM 37093 with Gemini South combined with simultaneous time-series photometry from Mt. John (New Zealand), SAAO, PROMPT, and Complejo Astronomico El Leoncito (CASLEO, Argentina). |
| publishDate |
2016 |
| dc.date.none.fl_str_mv |
2016 |
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info:eu-repo/semantics/publishedVersion info:eu-repo/semantics/conferenceObject Conferencia Journal http://purl.org/coar/resource_type/c_5794 info:ar-repo/semantics/documentoDeConferencia |
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http://hdl.handle.net/11336/138961 Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093; XXIX IAU General Assembly; Honolulu; Estados Unidos; 2015; 493-496 1743-9213 1743-9221 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/138961 |
| identifier_str_mv |
Constraining the physics of carbon crystallization through pulsations of a massive DAV BPM37093; XXIX IAU General Assembly; Honolulu; Estados Unidos; 2015; 493-496 1743-9213 1743-9221 CONICET Digital CONICET |
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eng |
| language |
eng |
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info:eu-repo/semantics/altIdentifier/doi/10.1017/S1743921316005962 info:eu-repo/semantics/altIdentifier/url/https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/constraining-the-physics-of-carbon-crystallization-through-pulsations-of-a-massive-dav-bpm37093/8D9F75390F58BA99E8BF8D6967B0202D |
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