Axions and the pulsation periods of variable white dwarfs revisited (Research Note)

Context. Axions are the natural consequence of the introduction of the Peccei-Quinn symmetry to solve the strong CP problem. All the efforts to detect such elusive particles have failed up to now. Nevertheless, it has been recently shown that the luminosity function of white dwarfs is best fitted if...

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Detalles Bibliográficos
Autores principales: Isern, J., García-Berro, E., Althaus, Leandro Gabriel, Córsico, Alejandro Hugo
Formato: Articulo
Lenguaje:Inglés
Publicado: 2010
Materias:
Ciencias Astronómicas
Elementary particles
Stars: oscillations
White dwarfs
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/82524
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-82524
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
Elementary particles
Stars: oscillations
White dwarfs
spellingShingle Ciencias Astronómicas
Elementary particles
Stars: oscillations
White dwarfs
Isern, J.
García-Berro, E.
Althaus, Leandro Gabriel
Córsico, Alejandro Hugo
Axions and the pulsation periods of variable white dwarfs revisited (Research Note)
topic_facet Ciencias Astronómicas
Elementary particles
Stars: oscillations
White dwarfs
description Context. Axions are the natural consequence of the introduction of the Peccei-Quinn symmetry to solve the strong CP problem. All the efforts to detect such elusive particles have failed up to now. Nevertheless, it has been recently shown that the luminosity function of white dwarfs is best fitted if axions with a mass of a few meV are included in the evolutionary calculations. Aims. Our aim is to show that variable white dwarfs can provide additional and independent evidence about the existence of axions. Methods. The evolution of a white dwarf is a slow cooling process that translates into a secular increase of the pulsation periods of some variable white dwarfs, the so-called DAV and DBV types. Since axions can freely escape from such stars, their existence would increase the cooling rate and, consequently, the rate of change of the periods as compared with the standard ones. Results. The present values of the rate of change of the pulsation period of G117-B15A are compatible with the existence of axions with the masses suggested by the luminosity function of white dwarfs, in contrast with previous estimations. Furthermore, it is shown that if such axions indeed exist, the drift of the periods of pulsation of DBV stars would be noticeably perturbed.
format Articulo
Articulo
author Isern, J.
García-Berro, E.
Althaus, Leandro Gabriel
Córsico, Alejandro Hugo
author_facet Isern, J.
García-Berro, E.
Althaus, Leandro Gabriel
Córsico, Alejandro Hugo
author_sort Isern, J.
title Axions and the pulsation periods of variable white dwarfs revisited (Research Note)
title_short Axions and the pulsation periods of variable white dwarfs revisited (Research Note)
title_full Axions and the pulsation periods of variable white dwarfs revisited (Research Note)
title_fullStr Axions and the pulsation periods of variable white dwarfs revisited (Research Note)
title_full_unstemmed Axions and the pulsation periods of variable white dwarfs revisited (Research Note)
title_sort axions and the pulsation periods of variable white dwarfs revisited (research note)
publishDate 2010
url http://sedici.unlp.edu.ar/handle/10915/82524
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