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Title: Gamma-ray bursts from the accretion of solid bodies onto high-velocity Galactic neutron stars

Abstract

We propose a simple model for the gamma-ray bursts based on high- velocity Galactic neutron stars that have accretion disks. The latter are formed from a mixture of material from the supernova shell and that ablated from a pre-supernova binary companion. Accretion onto the neutron star from this disk when the disk is still largely gaseous may result in a soft gamma-ray repeater phase. Much later, after the neutron star has moved away from its birthplace, solid bodies form in the disk, and some are perturbed into hitting the neutron star to create gamma-ray bursts. This model makes several predictions that are consistent with the observations. The observed combination of a high degree of isotropy on the sky coupled with the observed value of < V/V{sub max}> is not, at first glance, predicted, but is not impossible to attain in our model.

Authors:
;
Publication Date:
Research Org.:
Los Alamos National Lab., NM (United States)
Sponsoring Org.:
Department of Defense, Washington, DC (United States); National Aeronautics and Space Administration, Washington, DC (United States)
OSTI Identifier:
10113657
Report Number(s):
LA-UR-93-4340; CONF-9310252-4
ON: DE94005006
DOE Contract Number:
W-7405-ENG-36
Resource Type:
Conference
Resource Relation:
Conference: 2. gamma-ray burst workshop,Huntsville, AL (United States),20-22 Oct 1993; Other Information: PBD: [1993]
Country of Publication:
United States
Language:
English
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; NEUTRON STARS; COSMIC GAMMA BURSTS; STAR ACCRETION; SUPERNOVAE; GALAXIES; 661300; OTHER ASPECTS OF PHYSICAL SCIENCE

Citation Formats

Colgate, S.A., and Leonard, P.J.T.. Gamma-ray bursts from the accretion of solid bodies onto high-velocity Galactic neutron stars. United States: N. p., 1993. Web.
Colgate, S.A., & Leonard, P.J.T.. Gamma-ray bursts from the accretion of solid bodies onto high-velocity Galactic neutron stars. United States.
Colgate, S.A., and Leonard, P.J.T.. Fri . "Gamma-ray bursts from the accretion of solid bodies onto high-velocity Galactic neutron stars". United States. doi:. https://www.osti.gov/servlets/purl/10113657.
@article{osti_10113657,
title = {Gamma-ray bursts from the accretion of solid bodies onto high-velocity Galactic neutron stars},
author = {Colgate, S.A. and Leonard, P.J.T.},
abstractNote = {We propose a simple model for the gamma-ray bursts based on high- velocity Galactic neutron stars that have accretion disks. The latter are formed from a mixture of material from the supernova shell and that ablated from a pre-supernova binary companion. Accretion onto the neutron star from this disk when the disk is still largely gaseous may result in a soft gamma-ray repeater phase. Much later, after the neutron star has moved away from its birthplace, solid bodies form in the disk, and some are perturbed into hitting the neutron star to create gamma-ray bursts. This model makes several predictions that are consistent with the observations. The observed combination of a high degree of isotropy on the sky coupled with the observed value of < V/V{sub max}> is not, at first glance, predicted, but is not impossible to attain in our model.},
doi = {},
journal = {},
number = ,
volume = ,
place = {United States},
year = {Fri Dec 31 00:00:00 EST 1993},
month = {Fri Dec 31 00:00:00 EST 1993}
}

Conference:
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  • We propose a simple model for the gamma-ray bursts based on high-velocity Galactic neutron stars that have accretion disks. The latter are formed from a mixture of material from the supernova shell and that ablated from a pre-supernova binary companion. Accretion onto the neutron star from this disk when the disk is still largely gaseous may result in a soft gamma-ray repeater phase. Much later, after the neutron star has moved away from its birthplace, solid bodies form in the disk, and some are perturbed into hitting the neutron star to create gamma-ray bursts. This model makes several predictions thatmore » are consistent with the observations. The observed combination of a high degree of isotropy on the sky coupled with the observed value of [l angle][ital V]/[ital V][sub [ital max]][r angle] is not, at first glance, predicted, but is not impossible to attain in our model.« less
  • 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 themore » 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.« less
  • What makes a Galacic 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, {approximately}30My, after their formation. Our Galactic model for the isotropic component of (GBs) is based upon these high-velocity neutron stars (NSs) that have accretion disks. The fast NSs are formed in tidally locked binaries, where 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 formingmore » a slowly rotating NS. Following the collapse to a NS and explosion, subsequent accretion occurs on the rear side of the initially perturbed NS, resulting in a run-away acceleration of the neutron star 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 may be 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. Accretion onto the neutron star from this initially gaseous disk due to the ``alpha`` viscosity results initially in the soft gamma-ray repeater phase, {approximately}10{sup 4} yr. 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 21to22} g, are perturbed into being captured by the magnetic field of the NS to create GBs. The high velocity and millions of years delay in forming planetoids, results in isotropy.« less
  • These proceedings represent papers from the workshop on gamma{minus}ray bursters. The workshop was inspired by a major breakthrough in the understanding of gamma{minus}ray bursters. This advance was the linking of soft gamma{minus}ray repeaters with high velocity neutron stars. Topics discussed included supernovae, soft gamma{minus}ray repeaters, origins of high velocity neutron stars and radio observations of high velocity neutron stars. There are 48 papers presented at the workshop and 5 have been abstracted for the Energy Science and Technology database.(AIP)
  • 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, {approx}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 ({approx_gt}10{sup 3} kms{sup -1}) and slowly rotating (8 s) NSs. Tidal locking occurs due to the meridional circulation caused by the conservation of angularmore » 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 {approx}10{sup 4} yr. Later, after the neutron star has moved {approx}30 kpc from its birthplace, solid bodies form in the disk, and accrete to planetoid size bodies after {approx}3{times}10{sup 7} years. Some of these planetoid bodies, with a mass of {approx}10{sup 21}{endash}10{sup 22} g, are perturbed into an orbit inside the tidal distortion radius of {approx_gt}10{sup 5} km. Of these {approx}1% are captured by the magnetic field of the NS at R{lt}2{times}10{sup 3} km to create GBs.« less