A new mechanism for pulsar gamma-ray emission |
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Authors: | G. Z. Machabeli Qinghuan Luo D. B. Melrose S. Vladimirov |
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Affiliation: | Abastumani Astrophysical Observatory, Tbilisi 380060, Georgia; Department of Physics and Mathematical Physics, The University of Adelaide, SA 5005, Australia; Special Research Centre for Theoretical Astrophysics, School of Physics, The University of Sydney, NSW 2006, Australia; Department of Theoretical Physics, School of Physics, The University of Sydney, NSW 2006, Australia |
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Abstract: | Gamma-ray emission in pulsar magnetospheres is attributed to synchrotron radiation, which tends to decrease the pitch angle of the particle, being balanced by plasma processes tending to increase the pitch angle. The plasma processes are non-resonant instabilities that drive non-resonant quasilinear diffusion (NQD), thereby pumping energy from waves and the parallel motion of the particle into the perpendicular motion of the particle. It is shown that NQD can maintain the pitch angles for particles near the light-cylinder such that they radiate synchrotron radiation at MeV energies. Compared to conventional emission mechanisms (such as polar cap or outer gap models), the resulting spectrum has a relatively low upper cut-off from about a few to 100 MeV. Possible observational consequences of this mechanism are discussed. |
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Keywords: | plasmas radiation mechanisms: non-thermal pulsars: general gamma‐rays: theory |
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