Measuring the evolutionary rate of cooling of ZZ Ceti
- Autores
- Córsico, Alejandro Hugo; Romero, Alejandra Daniela
- Año de publicación
- 2013
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We have finally measured the evolutionary rate of cooling of the pulsating hydrogen atmosphere (DA) white dwarf ZZ Ceti (Ross 548), as reflected by the drift rate of the 213.13260694 s period. Using 41 yr of time-series photometry from 1970 November to 2012 January, we determine the rate of change of this period with time to be dP/dt = (5.2 ± 1.4) × 10-15 s s-1 employing the O-C method and (5.45 ± 0.79) × 10-15 s s-1 using a direct nonlinear least squares fit to the entire lightcurve. We adopt the dP/dt obtained from the nonlinear least squares program as our final determination, but augment the corresponding uncertainty to a more realistic value, ultimately arriving at the measurement of dP/dt = (5.5 ± 1.0) × 10-15 s s-1. After correcting for proper motion, the evolutionary rate of cooling of ZZ Ceti is computed to be (3.3 ± 1.1) × 10-15 s s-1. This value is consistent within uncertainties with the measurement of (4.19 ± 0.73) × 10-15 s s-1 for another similar pulsating DA white dwarf, G 117-B15A. Measuring the cooling rate of ZZ Ceti helps us refine our stellar structure and evolutionary models, as cooling depends mainly on the core composition and stellar mass. Calibrating white dwarf cooling curves with this measurement will reduce the theoretical uncertainties involved in white dwarf cosmochronometry. Should the 213.13 s period be trapped in the hydrogen envelope, then our determination of its drift rate compared to the expected evolutionary rate suggests an additional source of stellar cooling. Attributing the excess cooling to the emission of axions imposes a constraint on the mass of the hypothetical axion particle.
La lista completa de autores que integran el documento puede consultarse en el archivo.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
stars: evolution
stars: individual (ZZ Ceti, R548)
stars: oscillations (including pulsations)
stars: variables: general
white dwarfs - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/85098
Ver los metadatos del registro completo
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Measuring the evolutionary rate of cooling of ZZ CetiCórsico, Alejandro HugoRomero, Alejandra DanielaCiencias Astronómicasstars: evolutionstars: individual (ZZ Ceti, R548)stars: oscillations (including pulsations)stars: variables: generalwhite dwarfsWe have finally measured the evolutionary rate of cooling of the pulsating hydrogen atmosphere (DA) white dwarf ZZ Ceti (Ross 548), as reflected by the drift rate of the 213.13260694 s period. Using 41 yr of time-series photometry from 1970 November to 2012 January, we determine the rate of change of this period with time to be dP/dt = (5.2 ± 1.4) × 10<SUP>-15</SUP> s s<SUP>-1</SUP> employing the O-C method and (5.45 ± 0.79) × 10<SUP>-15</SUP> s s<SUP>-1</SUP> using a direct nonlinear least squares fit to the entire lightcurve. We adopt the dP/dt obtained from the nonlinear least squares program as our final determination, but augment the corresponding uncertainty to a more realistic value, ultimately arriving at the measurement of dP/dt = (5.5 ± 1.0) × 10<SUP>-15</SUP> s s<SUP>-1</SUP>. After correcting for proper motion, the evolutionary rate of cooling of ZZ Ceti is computed to be (3.3 ± 1.1) × 10<SUP>-15</SUP> s s<SUP>-1</SUP>. This value is consistent within uncertainties with the measurement of (4.19 ± 0.73) × 10<SUP>-15</SUP> s s<SUP>-1</SUP> for another similar pulsating DA white dwarf, G 117-B15A. Measuring the cooling rate of ZZ Ceti helps us refine our stellar structure and evolutionary models, as cooling depends mainly on the core composition and stellar mass. Calibrating white dwarf cooling curves with this measurement will reduce the theoretical uncertainties involved in white dwarf cosmochronometry. Should the 213.13 s period be trapped in the hydrogen envelope, then our determination of its drift rate compared to the expected evolutionary rate suggests an additional source of stellar cooling. Attributing the excess cooling to the emission of axions imposes a constraint on the mass of the hypothetical axion particle.La lista completa de autores que integran el documento puede consultarse en el archivo.Facultad de Ciencias Astronómicas y Geofísicas2013info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/85098enginfo:eu-repo/semantics/altIdentifier/issn/0004-637Xinfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/771/1/17info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:30Zoai:sedici.unlp.edu.ar:10915/85098Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:30.949SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Measuring the evolutionary rate of cooling of ZZ Ceti |
title |
Measuring the evolutionary rate of cooling of ZZ Ceti |
spellingShingle |
Measuring the evolutionary rate of cooling of ZZ Ceti Córsico, Alejandro Hugo Ciencias Astronómicas stars: evolution stars: individual (ZZ Ceti, R548) stars: oscillations (including pulsations) stars: variables: general white dwarfs |
title_short |
Measuring the evolutionary rate of cooling of ZZ Ceti |
title_full |
Measuring the evolutionary rate of cooling of ZZ Ceti |
title_fullStr |
Measuring the evolutionary rate of cooling of ZZ Ceti |
title_full_unstemmed |
Measuring the evolutionary rate of cooling of ZZ Ceti |
title_sort |
Measuring the evolutionary rate of cooling of ZZ Ceti |
dc.creator.none.fl_str_mv |
Córsico, Alejandro Hugo Romero, Alejandra Daniela |
author |
Córsico, Alejandro Hugo |
author_facet |
Córsico, Alejandro Hugo Romero, Alejandra Daniela |
author_role |
author |
author2 |
Romero, Alejandra Daniela |
author2_role |
author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas stars: evolution stars: individual (ZZ Ceti, R548) stars: oscillations (including pulsations) stars: variables: general white dwarfs |
topic |
Ciencias Astronómicas stars: evolution stars: individual (ZZ Ceti, R548) stars: oscillations (including pulsations) stars: variables: general white dwarfs |
dc.description.none.fl_txt_mv |
We have finally measured the evolutionary rate of cooling of the pulsating hydrogen atmosphere (DA) white dwarf ZZ Ceti (Ross 548), as reflected by the drift rate of the 213.13260694 s period. Using 41 yr of time-series photometry from 1970 November to 2012 January, we determine the rate of change of this period with time to be dP/dt = (5.2 ± 1.4) × 10<SUP>-15</SUP> s s<SUP>-1</SUP> employing the O-C method and (5.45 ± 0.79) × 10<SUP>-15</SUP> s s<SUP>-1</SUP> using a direct nonlinear least squares fit to the entire lightcurve. We adopt the dP/dt obtained from the nonlinear least squares program as our final determination, but augment the corresponding uncertainty to a more realistic value, ultimately arriving at the measurement of dP/dt = (5.5 ± 1.0) × 10<SUP>-15</SUP> s s<SUP>-1</SUP>. After correcting for proper motion, the evolutionary rate of cooling of ZZ Ceti is computed to be (3.3 ± 1.1) × 10<SUP>-15</SUP> s s<SUP>-1</SUP>. This value is consistent within uncertainties with the measurement of (4.19 ± 0.73) × 10<SUP>-15</SUP> s s<SUP>-1</SUP> for another similar pulsating DA white dwarf, G 117-B15A. Measuring the cooling rate of ZZ Ceti helps us refine our stellar structure and evolutionary models, as cooling depends mainly on the core composition and stellar mass. Calibrating white dwarf cooling curves with this measurement will reduce the theoretical uncertainties involved in white dwarf cosmochronometry. Should the 213.13 s period be trapped in the hydrogen envelope, then our determination of its drift rate compared to the expected evolutionary rate suggests an additional source of stellar cooling. Attributing the excess cooling to the emission of axions imposes a constraint on the mass of the hypothetical axion particle. La lista completa de autores que integran el documento puede consultarse en el archivo. Facultad de Ciencias Astronómicas y Geofísicas |
description |
We have finally measured the evolutionary rate of cooling of the pulsating hydrogen atmosphere (DA) white dwarf ZZ Ceti (Ross 548), as reflected by the drift rate of the 213.13260694 s period. Using 41 yr of time-series photometry from 1970 November to 2012 January, we determine the rate of change of this period with time to be dP/dt = (5.2 ± 1.4) × 10<SUP>-15</SUP> s s<SUP>-1</SUP> employing the O-C method and (5.45 ± 0.79) × 10<SUP>-15</SUP> s s<SUP>-1</SUP> using a direct nonlinear least squares fit to the entire lightcurve. We adopt the dP/dt obtained from the nonlinear least squares program as our final determination, but augment the corresponding uncertainty to a more realistic value, ultimately arriving at the measurement of dP/dt = (5.5 ± 1.0) × 10<SUP>-15</SUP> s s<SUP>-1</SUP>. After correcting for proper motion, the evolutionary rate of cooling of ZZ Ceti is computed to be (3.3 ± 1.1) × 10<SUP>-15</SUP> s s<SUP>-1</SUP>. This value is consistent within uncertainties with the measurement of (4.19 ± 0.73) × 10<SUP>-15</SUP> s s<SUP>-1</SUP> for another similar pulsating DA white dwarf, G 117-B15A. Measuring the cooling rate of ZZ Ceti helps us refine our stellar structure and evolutionary models, as cooling depends mainly on the core composition and stellar mass. Calibrating white dwarf cooling curves with this measurement will reduce the theoretical uncertainties involved in white dwarf cosmochronometry. Should the 213.13 s period be trapped in the hydrogen envelope, then our determination of its drift rate compared to the expected evolutionary rate suggests an additional source of stellar cooling. Attributing the excess cooling to the emission of axions imposes a constraint on the mass of the hypothetical axion particle. |
publishDate |
2013 |
dc.date.none.fl_str_mv |
2013 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion Articulo http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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article |
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publishedVersion |
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http://sedici.unlp.edu.ar/handle/10915/85098 |
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eng |
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eng |
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info:eu-repo/semantics/altIdentifier/issn/0004-637X info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/771/1/17 |
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info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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