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

This is the authors' abstract. We don't add key points for this paper.

We employ an asteroseismic model of L19-2, a relatively massive ( M ⋆ ∼ 0.75 M ⊙ ) and hot ( T eff ∼ 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 m a cos 2 β ≲ 25 meV or an axion-electron coupling constant of g ae ≲ 7 × 10 −13 .