Proton acceleration in neutron star magnetospheres

Details Proton acceleration in neutron star magnetospheres Proton acceleration in neutron star magnetospheres

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...388..148s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 388, March 20, 1992, p. 148-163.

Astronomy and Astrophysics

Astronomy

4

Neutron Stars, Particle Acceleration, Proton Energy, Stellar Magnetospheres, X Ray Binaries, Gamma Ray Astronomy, Hydrodynamic Equations, Magnetohydrodynamic Waves, Stellar Mass Accretion, Wave Generation

Scientific paper

To explain the emission of TeV and PeV gamma rays from accreting X-ray binary sources, protons must be accelerated to several times the gamma-ray energy. It is shown here that at certain times, the plasma in the accretion column of the neutron star may form a deep enough pool that the top portion becomes unstable to convective motions in spite of the strong magnetic field. The resulting turbulence produces fluctuations in the strength of the magnetic field that travel up the accretion column, taking energy out to the region of the energetic protons. The protons resonantly absorb this energy and are accelerated to high energies. Including the synchrotron radiation losses of the protons, it is shown that they can be accelerated to energies that are high enough to explain the gamma-ray observations.

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