Revisiting the axion bounds from the Galactic white dwarf luminosity function
- Autores
- Miller Bertolami, Marcelo Miguel; Melendez, Brenda Eliana; Althaus, Leandro Gabriel; Isern, J.
- Año de publicación
- 2014
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- It has been shown that the shape of the luminosity function of white dwarfs (WDLF) is a powerful tool to check for the possible existence of DFSZ-axions, a proposed but not yet detected type of weakly interacting particles. With the aim of deriving new constraints on the axion mass, we compute in this paper new theoretical WDLFs on the basis of WD evolving models that incorporate the feedback of axions on the thermal structure of the white dwarf. We find that the impact of the axion emission into the neutrino emission can not be neglected at high luminosities MBol ≲ 8 ) and that the axion emission needs to be incorporated self-consistently into the evolution of the white dwarfs when dealing with axion masses larger than ma cos2β ≳5 meV (i.e. axion-electron coupling constant gae 1.4× 10-13). We went beyond previous works by including 5 different derivations of the WDLF in our analysis. Then we have performed χ2-tests to have a quantitative measure of the agreement between the theoretical WDLFs - computed under the assumptions of different axion masses and normalization methods - - and the observed WDLFs of the Galactic disk. While all the WDLF studied in this work disfavour axion masses in the range suggested by asteroseismology ma cos2β 10 meV; gae 2.8× 10-13) lower axion masses can not be discarded from our current knowledge of the WDLF of the Galactic Disk. A larger set of completely independent derivations of the WDLF of the galactic disk as well as a detailed study of the uncertainties of the theoretical WDLFs is needed before quantitative constraints on the axion-electron coupling constant can be made.
Instituto de Astrofísica de La Plata
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
Axions
Dark matter detectors
Stars
White and brown dwarfs - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by/3.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/85024
Ver los metadatos del registro completo
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Revisiting the axion bounds from the Galactic white dwarf luminosity functionMiller Bertolami, Marcelo MiguelMelendez, Brenda ElianaAlthaus, Leandro GabrielIsern, J.Ciencias AstronómicasAxionsDark matter detectorsStarsWhite and brown dwarfsIt has been shown that the shape of the luminosity function of white dwarfs (WDLF) is a powerful tool to check for the possible existence of DFSZ-axions, a proposed but not yet detected type of weakly interacting particles. With the aim of deriving new constraints on the axion mass, we compute in this paper new theoretical WDLFs on the basis of WD evolving models that incorporate the feedback of axions on the thermal structure of the white dwarf. We find that the impact of the axion emission into the neutrino emission can not be neglected at high luminosities M<sub>Bol</sub> ≲ 8 ) and that the axion emission needs to be incorporated self-consistently into the evolution of the white dwarfs when dealing with axion masses larger than m<sub>a</sub> cos<sup>2</sup>β ≳5 meV (i.e. axion-electron coupling constant g<sub>ae</sub> 1.4× 10<sup>-13</sup>). We went beyond previous works by including 5 different derivations of the WDLF in our analysis. Then we have performed χ2-tests to have a quantitative measure of the agreement between the theoretical WDLFs - computed under the assumptions of different axion masses and normalization methods - - and the observed WDLFs of the Galactic disk. While all the WDLF studied in this work disfavour axion masses in the range suggested by asteroseismology m<sub>a</sub> cos<sup>2</sup>β 10 meV; g<sub>ae</sub> 2.8× 10-13) lower axion masses can not be discarded from our current knowledge of the WDLF of the Galactic Disk. A larger set of completely independent derivations of the WDLF of the galactic disk as well as a detailed study of the uncertainties of the theoretical WDLFs is needed before quantitative constraints on the axion-electron coupling constant can be made.Instituto de Astrofísica de La PlataFacultad de Ciencias Astronómicas y Geofísicas2014info: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/10915/85024enginfo:eu-repo/semantics/altIdentifier/issn/1475-7516info:eu-repo/semantics/altIdentifier/doi/10.1088/1475-7516/2014/10/069info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/3.0/Creative Commons Attribution 3.0 Unported (CC BY 3.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:20Zoai:sedici.unlp.edu.ar:10915/85024Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:21.145SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Revisiting the axion bounds from the Galactic white dwarf luminosity function |
title |
Revisiting the axion bounds from the Galactic white dwarf luminosity function |
spellingShingle |
Revisiting the axion bounds from the Galactic white dwarf luminosity function Miller Bertolami, Marcelo Miguel Ciencias Astronómicas Axions Dark matter detectors Stars White and brown dwarfs |
title_short |
Revisiting the axion bounds from the Galactic white dwarf luminosity function |
title_full |
Revisiting the axion bounds from the Galactic white dwarf luminosity function |
title_fullStr |
Revisiting the axion bounds from the Galactic white dwarf luminosity function |
title_full_unstemmed |
Revisiting the axion bounds from the Galactic white dwarf luminosity function |
title_sort |
Revisiting the axion bounds from the Galactic white dwarf luminosity function |
dc.creator.none.fl_str_mv |
Miller Bertolami, Marcelo Miguel Melendez, Brenda Eliana Althaus, Leandro Gabriel Isern, J. |
author |
Miller Bertolami, Marcelo Miguel |
author_facet |
Miller Bertolami, Marcelo Miguel Melendez, Brenda Eliana Althaus, Leandro Gabriel Isern, J. |
author_role |
author |
author2 |
Melendez, Brenda Eliana Althaus, Leandro Gabriel Isern, J. |
author2_role |
author author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas Axions Dark matter detectors Stars White and brown dwarfs |
topic |
Ciencias Astronómicas Axions Dark matter detectors Stars White and brown dwarfs |
dc.description.none.fl_txt_mv |
It has been shown that the shape of the luminosity function of white dwarfs (WDLF) is a powerful tool to check for the possible existence of DFSZ-axions, a proposed but not yet detected type of weakly interacting particles. With the aim of deriving new constraints on the axion mass, we compute in this paper new theoretical WDLFs on the basis of WD evolving models that incorporate the feedback of axions on the thermal structure of the white dwarf. We find that the impact of the axion emission into the neutrino emission can not be neglected at high luminosities M<sub>Bol</sub> ≲ 8 ) and that the axion emission needs to be incorporated self-consistently into the evolution of the white dwarfs when dealing with axion masses larger than m<sub>a</sub> cos<sup>2</sup>β ≳5 meV (i.e. axion-electron coupling constant g<sub>ae</sub> 1.4× 10<sup>-13</sup>). We went beyond previous works by including 5 different derivations of the WDLF in our analysis. Then we have performed χ2-tests to have a quantitative measure of the agreement between the theoretical WDLFs - computed under the assumptions of different axion masses and normalization methods - - and the observed WDLFs of the Galactic disk. While all the WDLF studied in this work disfavour axion masses in the range suggested by asteroseismology m<sub>a</sub> cos<sup>2</sup>β 10 meV; g<sub>ae</sub> 2.8× 10-13) lower axion masses can not be discarded from our current knowledge of the WDLF of the Galactic Disk. A larger set of completely independent derivations of the WDLF of the galactic disk as well as a detailed study of the uncertainties of the theoretical WDLFs is needed before quantitative constraints on the axion-electron coupling constant can be made. Instituto de Astrofísica de La Plata Facultad de Ciencias Astronómicas y Geofísicas |
description |
It has been shown that the shape of the luminosity function of white dwarfs (WDLF) is a powerful tool to check for the possible existence of DFSZ-axions, a proposed but not yet detected type of weakly interacting particles. With the aim of deriving new constraints on the axion mass, we compute in this paper new theoretical WDLFs on the basis of WD evolving models that incorporate the feedback of axions on the thermal structure of the white dwarf. We find that the impact of the axion emission into the neutrino emission can not be neglected at high luminosities M<sub>Bol</sub> ≲ 8 ) and that the axion emission needs to be incorporated self-consistently into the evolution of the white dwarfs when dealing with axion masses larger than m<sub>a</sub> cos<sup>2</sup>β ≳5 meV (i.e. axion-electron coupling constant g<sub>ae</sub> 1.4× 10<sup>-13</sup>). We went beyond previous works by including 5 different derivations of the WDLF in our analysis. Then we have performed χ2-tests to have a quantitative measure of the agreement between the theoretical WDLFs - computed under the assumptions of different axion masses and normalization methods - - and the observed WDLFs of the Galactic disk. While all the WDLF studied in this work disfavour axion masses in the range suggested by asteroseismology m<sub>a</sub> cos<sup>2</sup>β 10 meV; g<sub>ae</sub> 2.8× 10-13) lower axion masses can not be discarded from our current knowledge of the WDLF of the Galactic Disk. A larger set of completely independent derivations of the WDLF of the galactic disk as well as a detailed study of the uncertainties of the theoretical WDLFs is needed before quantitative constraints on the axion-electron coupling constant can be made. |
publishDate |
2014 |
dc.date.none.fl_str_mv |
2014 |
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 |
format |
article |
status_str |
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dc.identifier.none.fl_str_mv |
http://sedici.unlp.edu.ar/handle/10915/85024 |
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http://sedici.unlp.edu.ar/handle/10915/85024 |
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eng |
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info:eu-repo/semantics/altIdentifier/issn/1475-7516 info:eu-repo/semantics/altIdentifier/doi/10.1088/1475-7516/2014/10/069 |
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openAccess |
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