  We considered recently as a new axion production mechanism the process $e^-
\to e^- +a$ in a strong magnetic field $B$. Requiring that for a strongly
magnetized neutron star the axion luminosity is smaller than the neutrino
luminosity we obtained the bound $g_{ae} \lsim 10^{-10}$ for the axion electron
coupling constant. This limit is considerably weaker than the bound derived
earlier by Borisov and Grishina using the same method. Applying a similar
argument to magnetic white dwarf stars we obtained $g_{ae}\lsim 9 \cdot
10^{-13} (T/10^7)^{5/4} (B/10^{10})^{-2}$, where $T$ is the internal
temperature of the white dwarf. Here we note that the observed lack of
magnetized white dwarfs with low-temperature in the galactic disc could also be
interpreted as a signature of axion emission. Moreover, we speculate that axion
emission could explain why the putative galactic halo population of white
dwarfs is so dim.
