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We employ an asteroseismic model of L19-2, a relatively massive ($M_{\star}\sim 0.75 M_{\sun}$) and hot ($T_{\rm eff} \sim 12\,100$ K) pulsating DA(H-rich atmosphere) white dwarf star (DAV or ZZ Ceti variable), and use theobserved values of the temporal rates of period change of its dominantpulsation modes ($\Pi \sim 113$ s and $\Pi \sim 192$ s), to derive a newconstraint on the mass of the axion, the hypothetical non-barionic particleconsidered as a possible component of the dark matter of the Universe. If theasteroseismic model employed is an accurate representation of L19-2, then ourresults indicate hints of extra cooling in this star, compatible with emissionof axions of mass $m_{\rm a} \cos^2 \beta \lesssim 25$ meV or an axion-electroncoupling constant of $g_{\rm ae} \lesssim 7 \times 10^{-13}$.

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