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Neutron Star Mergers, Disks Around Black Holes, and Gamma-Ray Bursts

Published online by Cambridge University Press:  12 April 2016

H.-Th. Janka  and
M. Ruffert
H.-Th. Janka
Affiliation:
Max-Planck-Institut für Astrophysik, D-85740 Garching, Germany
M. Ruffert
Affiliation:
Max-Planck-Institut für Astrophysik, D-85740 Garching, Germany

Abstract

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We have performed three-dimensional hydrodynamical simulations of the coalescence of binary neutron stars taking into account the emission and backreaction of gravitational waves in the Newtonian code based on the “Piecewise Parabolic Method”. The use of the physical equation of state (EOS) of Lattimer & Swesty (1991) allowed us to calculate the production of neutrinos. We evaluated our models for the efficiency of v⊽ annihilation in the surroundings of the coalescing neutron stars. The corresponding energy deposition prior to and during merging turned out to be 2–3 orders of magnitude too small to power a typical γ-ray burst (GRB) with an energy output of ~ (1051/4π) erg/sterad at cosmological distances. Analytical estimates of the subsequent evolution of the disk which possibly surrounds the central black hole showed that even under the most favorable conditions the energy provided by v⊽ → e−e+ → γγ falls short by at least an order of magnitude. We discuss the implications of our results and speculate about possibilities how v⊽ annihilation might still be a viable energy source for GRBs.

Type
Part 8. X-Ray Binaries, Transients and Super-Soft Sources
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 384 - 387
Copyright
Copyright © Astronomical Society of the Pacific 1997

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