We study linear wave propagation in the case of equal-mass plasmas. We show that the special symmetry of such plasmas simplifies the problem and causes the disappearance of well-known phenomena such as Faraday rotation and whistler wave modes. We exploit the Symmetry of the problem to derive analytical expressions for wave propagation for various fluid models of the plasma. We also find which distribution functions will retain the symmetry properties of the fluid models.

We present a novel description of how energetic electrons may be ejected from the pulsar interior into the atmosphere, based on the collective electrostatic oscillations of interior electrons confined to move parallel to the magnetic field. The size of the interior magnetic field influences the interior plasma frequency, via the associated matter density compression. The plasma oscillations occur close to the regions of maximum magnetic field curvature, that is, close to the magnetic poles where the majority of magnetic flux emerges. Given that these oscillations have a density-dependent maximum amplitude before wave-breaking occurs, such waves can eject energetic electrons using only the self-field of the electron population in the interior. Moreover, photons emitted by electrons in the bulk of the oscillation can escape along the field lines by virtue of the lower opacity there (and the fact that they are emitted predominantly in this direction), leading to features in the spectra of pulsars.Comment: 8 pages, 1 figure, accepted for publication in MNRA

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The form of the propagating electrostatic Bernstein mode in a relativistic electron-positron plasma is markedly different from that in the classical plasma, once the momentum-dependent cyclotron frequency is accounted for in full inside the integrations. Given that particles in different parts of momentum space 'see' a different cyclotron frequency, there is no simple global singularity which reproduces the classical dispersion features.