Excitation of Alfven waves and pulsar radio emission

We analyse mechanisms of the excitation of Alfven waves in pulsar magnetospheres as a possible source of pulsar radio emission generation. We find that Cherenkov excitation of obliquely propagating Alfven 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 Alfven waves occurs in the kinetic regime still not very closed to the star: r greater than or equal to 50 R-NS. We also discuss various mechanisms of conversion of Alfven waves into escaping radiation. Unfortunately, no decisive conclusion about the effectiveness of such conversion can be made.