Computer Science
Scientific paper
Apr 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..366..269c&link_type=abstract
High velocity neutron stars and gamma-ray bursts. AIP Conference Proceedings, Volume 366, pp. 269-274 (1996).
Computer Science
3
Gamma-Ray Sources, Gamma-Ray Bursts, Neutron Stars, Stellar Content And Populations, Morphology And Overall Structure, Binary And Multiple Stars
Scientific paper
What makes a Galactic model of gamma-ray bursts (GBs) feasible is the observation of a new population of objects, fast neutron stars, that are isotropic with respect to the galaxy following a finite period, ~30 My, after their formation (1). Our Galactic model for the isotropic component of GBs is based upon high-velocity neutron stars (NSs) that have accretion disks. These fast NSs are formed in tidally locked binaries, producing a unique population of high velocity (>~103 km s-1 and slowly rotating (8 s) NSs. Tidal locking occurs due to the meridional circulation caused by the conservation of angular momentum of the tidal lobes. Following the collapse to a NS and the explosion, these lobes initially perturb the NS in the direction of the companion. Subsequent accretion (1 to 2 s) occurs on the rear side of the initial motion, resulting in a runaway acceleration of the NS by neutrino emission from the hot accreted matter. The recoil momentum of the relativistic neutrino emission from the localized, down flowing matter far exceeds the momentum drag of the accreted matter. The recoil of the NS is oriented towards the companion, but the NS misses because of the pre-explosion orbital motion. The near miss captures matter from the companion and forms a disk around the NS. Accretion onto the NS from this initially gaseous disk due to the ``alpha'' viscosity results in a soft gamma-ray repeater phase, which lasts ~104 yr. Later, after the neutron star has moved ~30 kpc from its birthplace, solid bodies form in the disk, and accrete to planetoid size bodies after ~3×107 years. Some of these planetoid bodies, with a mass of ~1021-1022 g, are perturbed into an orbit inside the tidal distortion radius of >~105 km. Of these ~1% are captured by the magnetic field of the NS at R<2×103 km to create GBs. The remainder either recirculate, are reprocessed, or are accreted in smaller mass units. The high velocity and millions of years delay in forming planetoids, results in isotropy. The depletion of planetoids by planet accretion after 108 years and the evolution of planetoid mass with time results in the observed value of
Colgate Stirling A.
Leonard Peter J. T.
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