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Several important mechanisms that explain the coherent pulsar radio emissionrely on streaming (or beam) instabilities of the relativistic pair plasma in apulsar magnetosphere. However, it is still not clear whether a streaminginstability by itself is sufficient to explain the observed coherent radioemission. Due to the relativistic conditions that are present in the pulsarmagnetosphere, kinetic instabilities could be quenched. Moreover, uncertaintiesregarding specific model-dependent parameters impede conclusions concerningthis question. We aim to constrain the possible parameter range for which astreaming instability could lead to pulsar radio emission, focusing on thetransition between strong and weak beam models, beam drift speed, andtemperature dependence of the beam and background plasma components. We solve alinear relativistic kinetic dispersion relation appropriate for pulsarconditions in a more general way than in previous studies, considering a widerparameter range. The analytical results are validated by comparison withrelativistic kinetic particle-in-cell (PIC) numerical simulations. We obtaingrowth rates as a function of background and beam densities, temperatures, andstreaming velocities while finding a remarkable agreement of the lineardispersion predictions and numerical simulation results in a wide parameterrange. Monotonous growth is found when increasing the beam-to-backgrounddensity ratio. With growing beam velocity, the growth rates firstly increase,reach a maximum and decrease again for higher beam velocities. A monotonousdependence on the plasma temperatures is found, manifesting in an asymptoticbehaviour when reaching colder temperatures. We show that the generated wavesare phase-coherent by calculating the fractional bandwidth. We provide anexplicit parameter range of plasma conditions for efficient pulsar radioemission.

Refining pulsar radio emission due to streaming instabilities: Linear theory and PIC simulations in a wide parameter range