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Session 74 - Pulsars.
Display session, Wednesday, January 15
The theory of the cyclotron-Cherenkov resonance in the pulsar magnetosphere is capable of explaining the main observational characteristics of pulsar radio emission. The maser-type instability is due to the interaction of the fast particles of the primary beam and from the tail of the distribution with the normal modes of a strongly magnetized one-dimensional electron-positron plasma at the anomalous Doppler resonance ømega(k)- k _II V_II + ømega_B/\gamma_res=0. In the emission process a resonant particle emits a wave undergoing transition to a higher rotational state producing coherent emission in core-like pattern. The conditions for the development of the cyclotron-Cherenkov instability are satisfied for the both typical and millisecond pulsars provided that the streaming energy of the bulk plasma is not very high \gamma_p = 5\div 10 or the relative streaming velocity of the electrons and positrons of bulk plasma is nonvanishing. In a curved magnetic field an instability at a drift-Cherenkov resonance ømega(k)- k _II V_II- k _\perp\, U_d may also produce a cone-like emission pattern.
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