Kinetic Dissipation of Pulsar Equatorial Stripe Wind and Particle Energization

Details Kinetic Dissipation of Pulsar Equatorial Stripe Wind and Particle Energization Kinetic Dissipation of Pulsar Equatorial Stripe Wind and Particle Energization

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21631506l&link_type=abstract

American Astronomical Society, AAS Meeting #216, #315.06; Bulletin of the American Astronomical Society, Vol. 41, p.895

Astronomy and Astrophysics

Astronomy

Scientific paper

Using 2-and-3-dimensional Particle-in-Cell codes, we simulate the kinetic dissipation of the equatorial stripe wind of obliquely spinning pulsars. We compute the internal conversion rate of electromagnetic energy into particle energy via self-generated current instabilities as the wind propagates. We also obtain the accelerated particle spectrum and emergent radiation. A nonthermal hard power law is produced in most cases. Our results will shed important new light on the so-called "Sigma problem": why are pulsar winds dominated by Poynting flux near the light cylinder but kinetic dominated near the termination shock.
Work supported by NSF grant AST-0909167

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