Pulsar radio emission mechanisms.

Details Pulsar radio emission mechanisms. Pulsar radio emission mechanisms.

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...189.7403l&link_type=abstract

American Astronomical Society, 189th AAS Meeting, #74.03; Bulletin of the American Astronomical Society, Vol. 28, p.1368

Astronomy and Astrophysics

Astronomy

Scientific paper

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 omega (k)- k II VII + omega_ {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 = 5/10 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 omega (k)- k II VII- k _{perpendicular to } U_d may also produce a cone-like emission pattern.

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