Quasilinear diffusion as a result of modulational instability in the pulsar plasma

Details Quasilinear diffusion as a result of modulational instability in the pulsar plasma Quasilinear diffusion as a result of modulational instability in the pulsar plasma

Mar 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002phrve..65c6408m&link_type=abstract

Physical Review E, vol. 65, Issue 3, id. 036408

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13

Relativistic Plasmas, Electron-Positron Plasmas, Plasma Turbulence, Nonlinear Phenomena: Waves, Wave Propagation, And Other Interactions

Scientific paper

Quasilinear diffusion due to modulational instability is considered in this paper. Interaction between the high-frequency, nearly transverse O mode (or the transverse X mode) and the low-frequency, nearly longitudinal L-O mode in a pulsar magnetospheric pair plasma can lead to modulational instability. The low-frequency L-O mode is superluminal, which is not subjected to usual Landau damping, and it is possible that excess wave energy is stored in this superluminal mode. The superluminal low-frequency L-O mode can dissipate in a way similar to the process of Langmuir wave collapse, that is, it cascades from the long- to short-wavelength regimes. When the phase speed becomes less than c, the waves can be damped through various resonances. We consider, in particular, damping through cyclotron resonance, which can lead to particle acceleration. The energetic beam particles, which have a very small spread initially, can develop a high-energy distribution tail, acquiring pitch angles through quasilinear diffusion. These particles can emit γ rays through synchrotron radiation, contributing to the observed pulsar high-energy emission.

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