Pulsed radiation from neutron star winds

Kirk, J. G.; Skjaeraasen, O.; Gallant, Y. A.

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Pulsed radiation from neutron star winds

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Kirk, J. G.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Skjaeraasen, O.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Gallant, Y. A.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Citation

Kirk, J. G., Skjaeraasen, O., & Gallant, Y. A. (2002). Pulsed radiation from neutron star winds. Astronomy & Astrophysics, 388(2), L29-L32.

Cite as: https://hdl.handle.net/11858/00-001M-0000-0011-8329-E

Abstract

The radiation of a pulsar wind is computed assuming that at roughly 10 to 100 light cylinder radii from the star, magnetic energy is dissipated into particle energy. The synchrotron emission of heated particles appears periodic, with, in general, both a pulse and an interpulse. The predicted spacing agrees well with the Crab and Vela pulse profiles. Using parameters appropriate for the Crab pulsar (magnetisation parameter at the light cylinder sigma(L) = 6 x 10(4), Lorentz factor Gamma = 250) agreement is found with the observed total pulsed luminosity. This suggests that the high-energy pulses from young pulsars originate not in the corotating magnetosphere within the light cylinder (as in all other models) but from the radially directed wind well outside it.