  One of the effective mechanisms of neutrino energy losses in red giants,
presupernovae and in the cores of white dwarfs is the emission of
neutrino-antineutrino pairs in the process of plasmon decay. In this paper, we
numerically calculate the emissivity due to plasmon decay in a wide range of
temperatures (10^7-10^11) K and densities (200-10^14) g cm^-3. Numerical
results are approximated by convenient analytical expressions. We also
calculate and approximate by analytical expressions the neutrino luminosity of
white dwarfs due to plasmon decay, as a function of their mass and internal
temperature. This neutrino luminosity depends on the chemical composition of
white dwarfs only through the parameter mu_e (the net number of baryons per
electron) and is the dominant neutrino luminosity in all white dwarfs at the
neutrino cooling stage.
