Streaming instability in relativistically hot pulsar magnetospheres

Details Streaming instability in relativistically hot pulsar magnetospheres Streaming instability in relativistically hot pulsar magnetospheres

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...428..261w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 428, no. 1, p. 261-266

Computer Science

Numerical Analysis

25

Astronomical Models, Counterflow, High Temperature Plasmas, Magnetohydrodynamic Flow, Pulsars, Radiation Transport, Relativistic Plasmas, Stability, Covariance, Maxwell Fluids, Numerical Analysis, Stellar Magnetic Fields

Scientific paper

Pulsar emission models often invoke wave instabilities in counterstreaming pair plasma as a mechanism to impose source coherence. The viability of the two-stream instability mechanism in a hot pair plasma, such as the one created by high-energy photons in a neutron star's magnetic field, is addressed in this paper. A two-stream dispersion relation is solved numerically, using a relativistic and covariant expression of the plasma dispersion function for a relativistic Maxwellian distribution. In the context of standard pulsar magnetospheric models, instability is demonstrated over the regions of P and P-dot parameter space in which most pulsars are found.

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