Physics
Scientific paper
May 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aipc..428..793r&link_type=abstract
Fourth Huntsville gamma-ray burst symposium. AIP Conference Proceedings, Volume 428, pp. 793-797 (1998).
Physics
1
Gamma-Ray Sources, Gamma-Ray Bursts, Neutron Stars, Elementary Particle Processes, Spectroscopic Binaries, Close Binaries
Scientific paper
We have simulated a variety of models, in order to shed light on the accessible physical conditions during the mergers, on the amount of matter dynamically ejected during the merging, on the timescales of mass accretion by the (forming) black hole, on the conversion of energy into neutrino emission, on the amount of energy deposited by νν-annihilation, and on the baryon loading of the created pair-plasma fireball. To this end, we varied the masses and mass ratios as well as the initial spins of the neutron stars, changed the impact parameter to consider spiral-in orbits and direct collisions, included a black hole (vacuum sphere) in our simulations, and studied the dynamical evolution of the accretion torus around the black hole formed after the neutron star merging until a (nearly) stationary state was reached. While the neutrino emission during the dynamical phases of the mergings is definitely too small to power gamma-ray bursts (GRBs), we find that the masses, lifetimes, and neutrino luminosities of the accretion tori have values that might explain short (O(0.1-1 s)) and not too powerful (~1051/(4π)erg/(s.sterad)) gamma-ray bursts.
Janka Hans-Thomas
Ruffert Maximilian
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