An asteroseismic constraint on the mass of the axion from the period drift of the pulsating DA white dwarf star L19-2

Abstract

We employ an asteroseismic model of L19-2, a relatively massive ($M_{\star} \sim 0.75 M_{\sun}$) and hot ($T_{\mathrm{eff}}\sim 12100$ 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 ($\Pi \sim 113$ s and $\Pi \sim 192$ 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 $m_{\mathrm{a}}{\cos }^2\beta \lesssim 25$ meV or an axion-electron coupling constant of $g_{\mathrm{ae}}\lesssim 7\times 10^{-13}$.

20 pages, 6 figures, 3 tables. Revised version. Accepted for publication in the Journal of Cosmology and Astroparticle Physics. arXiv admin note: text overlap with arXiv:1205.6180

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