Proton acceleration in neutron star magnetospheres

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

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991aipc..220..232s&link_type=abstract

High Energy Gamma-Ray Astronomy. AIP Conference Proceedings, Volume 220, pp. 232-236 (1991).

Astronomy and Astrophysics

Astronomy

1

X-Ray Binaries, Gamma-Ray Sources, Gamma-Ray Bursts, Neutron Stars

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 was proposed that protons could be accelerated to these energies in the outer regions of a neutron star's closed magnetosphere. We show here, that at certain times, the plasma in the accretion column of the neturon 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 to 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, we have found that they can be accelerated to energies that are high enough to explain the gamma-ray observations.

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