  We compute the emission of gravitational radiation from pulsating white
dwarfs. This is done by using an up-to-date stellar evolutionary code coupled
with a state-of-the-art pulsational code. The emission of gravitational waves
is computed for a standard 0.6 solar masses white dwarf with a liquid
carbon-oxygen core and a hydrogen-rich envelope, for a massive DA white dwarf
with a partially crystallized core for which various l=2 modes have been
observed (BPM 37093) and for PG 1159-035, the prototype of the GW Vir class of
variable stars, for which several quadrupole modes have been observed as well.
We find that these stars do not radiate sizeable amounts of gravitational waves
through their observed pulsation g-modes, in line with previous studies. We
also explore the possibility of detecting gravitational waves radiated by the
f-mode and the p-modes. We find that in this case the gravitational wave signal
is very large and, hence, the modes decay very rapidly. We also discuss the
possible implications of our calculations for the detection of gravitational
waves from pulsating white dwarfs within the framework of future space-borne
interferometers like LISA.
