Relativistic shocks in electron-positron plasmas and polar cap accretion onto neutron stars: Two non-linear problems in astrophysical plasma physics

Details Relativistic shocks in electron-positron plasmas and polar cap accretion onto neutron stars: Two non-linear problems in astrophysical plasma physics Relativistic shocks in electron-positron plasmas and polar cap accretion onto neutron stars: Two non-linear problems in astrophysical plasma physics

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989plap.work..117a&link_type=abstract

In ESA, Proceedings of an International School and Workshop on Plasma Astrophysics, Volume 1 p 117-124 (SEE N89-24910 18-75)

Astronomy and Astrophysics

Astrophysics

Neutron Stars, Plasma Waves, Relativistic Plasmas, Shock Waves, Space Plasmas, Stellar Mass Accretion, Astronomical Models, Particle Acceleration, Plasma-Particle Interactions

Scientific paper

Particle simulations and theory of relativistic shock waves in an e+ e- plasma simulation are outlined. Magnetic reflection of particles is an essential role in the shock structure. Instability of the reflected particles in the shock front produces intense extraordinary mode radiation. Such shocks are candidates for the particle accelerator in plerions and in extragalactic jets only if the upstream Poynting flux composes no more than 10 percent of the total. Analytical and numerical studies of radiation dominated accretion onto the magnetic poles of neutron stars are summarized. The upper limit to the photon luminosity depends upon magnetic confinement, not upon the dragging of photons into the star. Numerical solutions show the plasma forms large scale photon bubbles. The percolative loss of radiation controls the pressure and therefore the limits of magnetic confinement. Loss of magnetic confinement through resistive interchange instability is suggested as a means of generating TeV to PeV voltage drops along the magnetic field.

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