Precessing Gamma Jets in the extended and evaporating galactic halo as the sources of GRBs

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Abstract
Precessing Gamma Jets (GJ) in binary systems located in extended or evaporating galactic halos should be the sources of GRBs. The GJ are born by Inverse Compton Scattering (ICS) of thermal photons (optical, infrared,…) onto (power law) electron jets (from GeV energies and above) produced by spinning pulsars or black holes. The thermal photons are emitted by the binary companion (or by their nearby accreting disk). The collimated GJ beam is trembling with the characteristic pulsar millisecond period and it is bent by the companion magnetic field interactions, as a lighthouse, in a nearly conical shape within the characteristic Keplerian period; an additional nutation due to the asymmetric inertial momentum may lead, in general, to aperiodic behaviour of GRB signals. SGRs are GRBs seen at the periphery of the hard energy GJ beam core. The original birth locations of GJ (SNRs, planetary nebulae, globular clusters,…) are smeared out by the high escape velocity of the system; the Neutron Star (NS) high velocity is possibly due to the asymmetric jet precession, and consequent “rowing” acceleration, related to the eccentricity of the binary system. The GJ power is, for realistic parameters, comparable to that needed for GRBs in an extended or evaporating galactic halo. Their detailed spectra and time evolution fit the observed data. The expected GRB source number (within present BATSE sensitivity) is tens of thousands, compatible with the allowed presence of 10–20% GRB repeaters.
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