Three-wave turbulence in pulsar winds

Details Three-wave turbulence in pulsar winds Three-wave turbulence in pulsar winds

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..154..187l&link_type=abstract

Solar Physics, vol. 154, no. 1, p. 187-198

Astronomy and Astrophysics

Astronomy

9

Brightness Temperature, Cyclotron Resonance, Interstellar Gas, Interstellar Magnetic Fields, Radio Astronomy, Radio Emission, Radio Occultation, Radio Scattering, Radio Sources (Astronomy), Stellar Winds, Wave Interaction, Compton Effect, Diffusion Coefficient, Kinetic Equations, Magnetization, Magnetohydrodynamic Stability, Mathematical Models, Nonlinearity, Photon-Electron Interaction, Photons, Plasma Temperature, Raman Spectra

Scientific paper

Three-wave interactions can modify the very bright radio waves propagating through dense, magnetized pulsar winds and prevent radiation from escaping, or severely alter the resulting spectrum. Absence of the signatures of such effects in the very bright radio emission from pulsars implies constraints on the structure of their winds, especially for a spherically-symmetric wind which should block the radiation unless the Lorentz factor of the pairs is much greater than 8 x 102.

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