Stability of a relativistic rotating electron-positron jet: Non-axisymmetric perturbations

We investigate the linear stability of a hydrodynamic relativistic flow of magnetized plasma in the simplest case where the energy density of the electromagnetic fields is much greater than the energy density of the matter (including the rest mass energy). This is the force-free approximation. We consider the case of a light cylindrical jet in a cold and dense environment, so that the jet boundary remains at rest, Continuous and discrete spectra of frequencies are investigated analytically. An infinite sequence of eigenfrequencies is found near the edge of the Alfven continuum. Numerical calculations show that modes having reasonable values of azimuthal wavenumber m and radial number n are stable and their attenuation increment gamma is small. The dispersion curves omega = omega(k(parallel to)) have a minimum for k(parallel to 0) similar or equal to 1/R (R is the jet radius), This results in the accumulation of perturbations inside the jet with wavelengths of the order of the jet radius. The wave crests of the perturbation pattern formed in such a way move along the jet with a velocity exceeding the speed of light, If one has relativistic electrons emitting synchrotron radiation inside the jet, then this pattern will be visible, This provides us with a new type of superluminal source, If the jet is oriented close to the line of sight, then the observer will see knots moving backward to the core.