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HK: Hadronen und Kerne
HK 50: Nukleare Astrophysik III
HK 50.3: Talk
Wednesday, March 26, 1997, 17:45–18:00, HS D
Merging neutron stars — •Stephan Rosswog1, Matthias Liebendoerfer1, Friedrich-Karl Thielemann1, Willy Benz2, and Melvyn Davies3 — 1Department of Physics and Astronomy, University of Basel — 2Steward Observatory, University of Arizona — 3Institute of Astronomy, University of Camebridge
We investigate the coalescence of two neutron stars of equal mass as final state of a neutron star binary system, that loses angular momentum through emission of gravitational radiation. The coalescence results in a very massive central object (that will very probably collapse to a black hole on a time scale depending on the used microphysics), surrounded by a disk and spiral arms consisting of hot nuclear matter. The hydrodynamical simulations are carried out using a 3D Newtonian SPH-code. We use the equation of state for hot nuclear matter of Lattimer and Swesty (s.[1]) in a tabulated form. In the hydrodynamical energy equation we take source terms resulting from changes in the nuclear binding energies and from energy losses through neutrino transport into account. We discuss the final states of (observable) binary pulsars, a possible connection with gamma ray bursts (at cosmological distances) and a possible contribution to the production of r-process elements.
[1]: Lattimer J.M., Swesty F.D., 1991, Nucl. Phys. A 535, 331 [2]: Davies M.B. et al., 1994, ApJ 431, 742