Ultra-high energy cosmic ray acceleration by accretion-induced collapse pulsars in the local universe

Details Ultra-high energy cosmic ray acceleration by accretion-induced collapse pulsars in the local universe Ultra-high energy cosmic ray acceleration by accretion-induced collapse pulsars in the local universe

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icrc....6.2105d&link_type=abstract

Proceedings of the 27th International Cosmic Ray Conference. 07-15 August, 2001. Hamburg, Germany. Under the auspices of the Int

Physics

1

Scientific paper

We discuss the possibility that the ultra-high energy cosmic rays (UHECRs) observed above the GZK limit could be mostly protons accelerated in magnetic reconnection sites just above the magnetosphere of newborn millisecond pulsars originated by accretion-induced-collapse (AICpulsars). We find that the observed total flux of UHECRs can be produced by the integrated contribution from all AICpulsars of the local distribution of galaxies within a distance which is unaffected by the GZK cutoff (< 50 Mpc) (de Gouveia Dal Pino & Lazarian 2000). We also examine the potential acceleration mechanisms in the reconnection site and find that first-order Fermi acceleration cannot provide either sufficient efficiency (due to synchrotron losses) or the expected spectral index for the UHECR particle spectrum. This leaves the one-shot acceleration via an induced electric field within the reconnection region as the only viable process for UHECR acceleration. We find that AIC-pulsars with surface magnetic fields 1012 - 1015 G, and spin periods ˜ 1 - 60 ms, are able to accelerate particles to energies > 1020 eV, but the magnetic field just above the Alfv´en surface must be predominantly toroidal for the particles to be allowed to escape from the acceleration zone without being deflected. Synchrotron losses impose important constraints on the magnetic field topology of any UHECR accelerators involving compact sources with strong magnetic fields.

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