Coalescing neutron stars as gamma-ray bursters?

Ruffert, M.; Janka, Hans‐Thomas; Schäfer, Gerhard

doi:10.1063/1.51657

Cited by 215 publications

(462 citation statements)

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“…GW emission and its back-reaction on the hydrodynamics were taken into account by the method of Blanchet, Damour, & Schäfer (1990;see also Ruffert, Janka, & Schäfer 1996). The neutrino emission and corresponding energy and lepton number changes of the matter were calculated with an elaborate neutrino leakage scheme (Ruffert et al 1996), and annihilation around the merger was evaluated in a postpronn cessing step (Ruffert et al 1997). Table 1 gives a list of computed NS/NS and BH/NS merger models.…”

Section: Methodsmentioning

confidence: 99%

“…Besides the baryonic mass of the neutron star and the mass of the black hole, the spins of the neutron stars were varied. The cool neutron stars have a radius of about 15 km (Ruffert et al 1996), and the runs were started with a centerto-center distance of [42][43][44][45][46] Note.-"Solid" means synchronously rotating stars, "none" denotes irrotational cases, and "anti" is for counterrotation, i.e., spin vectors opposite to the direction of the orbital angular momentum. a 1 foe = 10 51 ergs.…”

Section: Methodsmentioning

confidence: 99%

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Black Hole–Neutron Star Mergers as Central Engines of Gamma-Ray Bursts

Janka

Eberl

Ruffert

et al. 1999

The Astrophysical Journal

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Hydrodynamic simulations of the merger of stellar mass black hole-neutron star binaries are compared with mergers of binary neutron stars. The simulations are Newtonian but take into account the emission and backreaction of gravitational waves. The use of a physical nuclear equation of state allows us to include the effects of neutrino emission. For low neutron star-to-black hole mass ratios, the neutron star transfers mass to the black hole during a few cycles of orbital decay and subsequent widening before finally being disrupted, whereas for ratios near unity the neutron star is destroyed during its first approach. A gas mass between ∼0.3 and ∼0.7 M , is left in an accretion torus around the black hole and radiates neutrinos at a luminosity of several times 10 53 ergs s Ϫ1 during an estimated accretion timescale of about 0.1 s. The emitted neutrinos and antineutrinos annihilate into e ‫ע‬ pairs with efficiencies of 1%-3% and rates of up to ∼ ergs s Ϫ1 , thus depositing an energy 52 2 # 10 ergs above the poles of the black hole in a region that contains less than 10 Ϫ5 M , of baryonic matter.

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Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

Black Hole–Neutron Star Mergers as Central Engines of Gamma-Ray Bursts

Janka

Eberl

Ruffert

et al. 1999

The Astrophysical Journal

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255

313

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“…To this end the 3D Newtonian equations of hydrodynamics were integrated by the Riemann-solver based "Piecewise Parabolic Method" (Colella & Woodward 1984) on an equidistant Cartesian grid with a resolution of 64x64x32 or 128 X 128 X 64 zones. The effects of the backreaction of gravitational waves on the hydrodynamic flow were included (see Ruffert et al 1996a). The properties of neutron star matter were described by the EOS of Lattimer & Swesty (1991).…”

Section: Numerical Approachmentioning

confidence: 99%

“…The properties of neutron star matter were described by the EOS of Lattimer & Swesty (1991). Energy loss and changes of the electron abundance due to the emission of v's were taken into account by an elaborate "neutrino leakage scheme" that was calibrated using diffusion results (Ruffert et al 1996a). Neutrinos of all types are produced by thermal processes and v e and v e also by the /3-processes.…”

Section: Numerical Approachmentioning

confidence: 99%

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

Janka

Ruffert

1997

International Astronomical Union Colloquium

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Abstract.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 vv 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 7-ray burst (GRB) with an energy output of ~ (10 51 /47r) 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 vv -> e~e + -»• 77 falls short by at least an order of magnitude. We discuss the implications of our results and speculate about possibilities how vv annihilation might still be a viable energy source for GRBs.

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The Final Fate of Coalescing Binary Neutron Stars: Collapse to a Black Hole?

Rasio

Black Holes in Binaries and Galactic Nuclei: Diagnostics, Demography and Formation

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Abstract. Coalescing compact binaries with neutron star (NS) or black hole (BH) components are important sources of gravitational waves for the laser-interferometer detectors currently under construction, and may also be sources of gamma-ray bursts at cosmological distances. This paper focuses on the final hydrodynamic coalescence and merger of NS-NS binaries, and addresses the question of whether black hole formation is the inevitable final fate of these systems.

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Coalescing neutron stars as gamma-ray bursters?

Cited by 215 publications

References 1 publication

Black Hole–Neutron Star Mergers as Central Engines of Gamma-Ray Bursts

Black Hole–Neutron Star Mergers as Central Engines of Gamma-Ray Bursts

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

The Final Fate of Coalescing Binary Neutron Stars: Collapse to a Black Hole?

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