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
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/85024

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network_name_str SEDICI (UNLP)
spelling 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
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info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/85024
url http://sedici.unlp.edu.ar/handle/10915/85024
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/1475-7516
info:eu-repo/semantics/altIdentifier/doi/10.1088/1475-7516/2014/10/069
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/3.0/
Creative Commons Attribution 3.0 Unported (CC BY 3.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/3.0/
Creative Commons Attribution 3.0 Unported (CC BY 3.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
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instname_str Universidad Nacional de La Plata
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repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
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