The rate of cooling of the pulsating white dwarf star G117-B15A: A new asteroseismological inference of the axion mass

dc.creatorCórsico, Alejandro Hugo
dc.creatorAlthaus, Leandro Gabriel
dc.creatorMiller Bertolami, Marcelo Miguel
dc.creatorRomero, Alejandra Daniela
dc.creatorGarcía-Berro, E.
dc.creatorIsern, J.
dc.creatorKepler, S. O.
dc.date2012
dc.date2019-10-31T17:06:00Z
dc.identifierhttp://sedici.unlp.edu.ar/handle/10915/84570
dc.identifierissn:0035-8711
dc.descriptionWe employ a state-of-the-art asteroseismological model of G117-B15A, the archetype of the H-rich atmosphere (DA) white dwarf pulsators (also known as DAV or ZZ Ceti variables), and use the most recently measured value of the rate of period change for the dominant mode of this pulsating star to derive a new constraint on the mass of axion, the still conjectural non-baryonic particle considered as a candidate for dark matter of the Universe. Assuming that G117-B15A is truly represented by our asteroseismological model, and, in particular, that the period of the dominant mode is associated with a pulsation g mode trapped in the H envelope, we find strong indications of the existence of extra cooling in this star, compatible with emission of axions of mass macos2β=17.4-2.7+2.3 meV.
dc.descriptionFacultad de Ciencias Astronómicas y Geofísicas
dc.formatapplication/pdf
dc.format2792-2799
dc.languageen
dc.rightshttp://creativecommons.org/licenses/by-nc-sa/4.0/
dc.rightsCreative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.subjectCiencias Astronómicas
dc.subjectAsteroseismology
dc.subjectElementary particles
dc.subjectStars: individual: ZZ Ceti stars
dc.subjectStars: interiors
dc.subjectStars: oscillations
dc.subjectWhite dwarfs
dc.titleThe rate of cooling of the pulsating white dwarf star G117-B15A: A new asteroseismological inference of the axion mass
dc.typeArticulo
dc.typeArticulo


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