Gamma-ray emission in relativistic pulsar magnetospheric plasmas

Details Gamma-ray emission in relativistic pulsar magnetospheric plasmas Gamma-ray emission in relativistic pulsar magnetospheric plasmas

Oct 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aipc..587..585l&link_type=abstract

GAMMA 2001: Gamma-Ray Astrophysics 2001. AIP Conference Proceedings, Volume 587, pp. 585-589 (2001).

Astronomy and Astrophysics

Astrophysics

2

Pulsars, Gamma-Ray Sources, Gamma-Ray Bursts, Magnetohydrodynamics And Plasmas

Scientific paper

We consider γ-ray emission as the result of plasma instabilities. The pulsar magnetosphere is populated with an outflowing relativistic pair plasma, which contains a fast energetic particle beam. Such a system is well known to be unstable with certain types of plasma instabilities being able to develop, leading to quasilinear diffusion. Due to such diffusion, particles initially in the ground Landau state can acquire pitch angles so that they can emit cyclotron/synchrotron radiation. This process should contribute to the observed high energy spectrum in addition to that from the widely discussed synchrotron-cascade process. Application of this mechanism to high energy emission from both normal young pulsars and millisecond pulsars is discussed. .

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