Physics
Scientific paper
Nov 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..dppfo1009w&link_type=abstract
American Physical Society, 44th Annual Meeting of the Division of Plasma , abstract #FO1.009
Physics
Scientific paper
A relativistic pair-plasma which contains a high excitation of electrostatic turbulence can produce intense maser radiation by stimulated Compton scattering. Because conditions suited to the maser are possible in the magnetosphere of a pulsar, such a maser may be responsible for observed radio emission. If the plasma is moving relative to the lab/star frame because of the polar cap current flow, the emission will be relativistically beamed. One interesting consequence of the moving maser is that the angle of the peak emission relative to the current flow is a function of frequency. Radio pulsars, in fact, do show a variation in pulse profile (intensity vs. phase) at different observing frequencies. This is generally interpreted as radius-to-frequency mapping, according to the presumption that the emission comes from different heights in the polar cap, and that the emission frequency is tied to the local plasma frequency. Maser emission from a single location can produce similar frequency-dependent profiles.
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