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Title:
High-resolution calculations of merging neutron stars - III. Gamma-ray bursts
Authors:
Rosswog, Stephan; Ramirez-Ruiz, Enrico; Davies, Melvyn B.
Affiliation:
AA(Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH), AB(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AC(Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 345, Issue 4, pp. 1077-1090. (MNRAS Homepage)
Publication Date:
11/2003
Origin:
MNRAS
Astronomy Keywords:
dense matter, hydrodynamics, neutrinos, methods: numerical, stars: neutron, gamma-rays: bursts
DOI:
10.1046/j.1365-2966.2003.07032.x
Bibliographic Code:
2003MNRAS.345.1077R

Abstract

Recent three-dimensional, high-resolution simulations of neutron star coalescences are analysed to assess whether short gamma-ray bursts (GRBs) could originate from such encounters. The two most popular modes of energy extraction - namely the annihilation of and magnetohydrodynamic processes - are explored in order to investigate their viability in launching GRBs. We find that annihilation can provide the necessary stresses to drive a highly relativistic expansion. However, unless the outflow is beamed into less than 1 per cent of the solid angle, this mechanism may fail to explain the apparent isotropized energies implied for short GRBs at cosmological distances. We argue that the energetic, neutrino-driven wind that accompanies the merger event will have enough pressure to provide adequate collimation to the -annihilation-driven jet, thereby comfortably satisfying constraints on event rate and apparent luminosity. We also assess magnetic mechanisms to transform the available energy into a GRB. If the central object does not collapse immediately into a black hole, it will be convective and it is expected to act as an effective large scale dynamo, amplifying the seed magnetic fields to a few times 1017 G within a small fraction of a second. The associated spindown time-scale is 0.2 s, coinciding with the typical duration of a short GRB. The efficiencies of the various assessed magnetic processes are high enough to produce isotropized luminosities in excess of 1052 erg s-1 even without beaming.

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