Gamma-ray bursts from planetoid accretion onto fast galactic neutron stars

We propose a Galactic model for the isotropic component of gamma-my bursts (GB`s) based upon high-velocity neutron stars (NS`s) that have accretion disks. The fast NS`s are formed in tidally locked binaries, leading to a unique fast NS population. The tidal locking occurs due to the meridional circulation caused by the conservation of angular momentum of the tidal lobes. These same lobes perturb the subsequent collapse to a supernova and a slowly rotating NS. Following the collapse and explosion, subsequent accretion occurs on the rear side of the initially perturbed NS. A resulting instability leads to run-away acceleration of the neutron star by neutrino emission from the hot accreted matter. The recoil of the NS is oriented towards the companion, but misses because of the initial orbital motion. The near miss captures matter from the companion and forms a disk around the NS. The disk material is captured from the material ablated from a pre-supernova binary companion. Accretion onto the neutron star from this initially gaseous disk due to the enhanced ``alpha`` viscosity results initially in the soft gamma-ray repeater phase, {approximately}10{sup 4} y. Later, after the neutron star has moved {approximately}30 kpc from its birthplace, solid bodies form in the disk, and accrete to planetoid size bodies after {approximately}3 {times} 10{sup 7} years. Some of these planetoid bodies, with a mass of {approximately}10{sup 21--22} g, are perturbed into being captured by the magnetic field of the NS to create gamma-ray bursts. The high velocity and millions of years delay in forming planetoids, results in galactic isotropy. The depletion of planetoids by planet accretion after 10{sup 8} years and the evolution of planetoid mass with time results in the observed value of V/V{sub max}. The hard spectrum is produced by the collision with, twisting, and ultimately the reconnection, of the NS magnetic field