  We analyze mechanisms of the excitation of Alfv\'{e}n wave in pulsar
magnetospheres as a possible source of pulsar radio emission generation. We
find that Cherenkov excitation of obliquely propagating Alfv\'{e}n waves is
inefficient, while excitation at the anomalous cyclotron resonance by the
particles from the primary beam and from the tail of the bulk distribution
function may have a considerable growth rate. The cyclotron instability on
Alfv\'{e}n waves occurs in the kinetic regime still not very closed to the
star: $r \geq 50 R_{NS}$. We also discuss various mechanisms of conversion of
Alfv\'{e}n waves into escaping radiation. Unfortunately, no decisive conclusion
about the effectiveness of such conversion can be made.
