An asteroseismic constraint on the mass of the axion from the period drift of the pulsating DA white dwarf star L19-2
We employ an asteroseismic model of L19-2, a relatively massive M? ∼ 0.75M and hot (Teff ∼ 12 100 K) pulsating DA (H-rich atmosphere) white dwarf star (DAV or ZZ Ceti variable), and use the observed values of the temporal rates of period change of its dominant pulsation modes (Π ∼ 113 s and Π ∼ 19...
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| Autores principales: | , , , , , , , , |
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| Formato: | Articulo |
| Lenguaje: | Inglés |
| Publicado: |
2016
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| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/93643 http://iopscience.iop.org/article/10.1088/1475-7516/2016/07/036/meta |
| Aporte de: |
| Sumario: | We employ an asteroseismic model of L19-2, a relatively massive M? ∼ 0.75M and hot (Teff ∼ 12 100 K) pulsating DA (H-rich atmosphere) white dwarf star (DAV or ZZ Ceti variable), and use the observed values of the temporal rates of period change of its dominant pulsation modes (Π ∼ 113 s and Π ∼ 192 s), to derive a new constraint on the mass of the axion, the hypothetical non-barionic particle considered as a possible component of the dark matter of the Universe. If the asteroseismic model employed is an accurate representation of L19-2, then our results indicate hints of extra cooling in this star, compatible with emission of axions of mass ma cos2 β . 25 meV or an axion-electron coupling constant of gae . 7×10−13 |
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