Excitation of Alfven Waves and Pulsar Radio Emission

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: $r\ge 50R_{NS}$. 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.