SIMBAD references

We investigate systematically the dynamical mass ejection, r-process nucleosynthesis, and properties of electromagnetic counterparts of neutron-star (NS) mergers in dependence on the uncertain properties of the nuclear equation of state (EOS) by employing 40 representative, microphysical high-density EOSs in relativistic, hydrodynamical simulations. The crucial parameter determining the ejecta mass is the radius R_1.35 of a 1.35 M_☉NS. NSs with smaller R_1.35("soft" EOS) eject systematically higher masses. These range from ∼10^–3 M_☉ to ∼10^–2 M_☉for 1.35-1.35 M_☉ binaries and from ∼5x10^–3 M_☉ to ∼2x10^–2 M_☉for 1.2-1.5 M_☉ systems (with kinetic energies between ∼5x10⁴⁹ erg and 10⁵¹ erg). Correspondingly, the bolometric peak luminosities of the optical transients of symmetric (asymmetric) mergers vary between 3x10⁴¹ erg/s and 14x10⁴¹ erg/s (9x10⁴¹ erg/s and 14.5x10⁴¹ erg/s) on timescales between ∼2 hr and ∼12 hr. If these signals with absolute bolometric magnitudes from -15.0 to -16.7 are measured, the tight correlation of their properties with those of the merging NSs might provide valuable constraints on the high-density EOS. The r-process nucleosynthesis exhibits a remarkable robustness independent of the EOS, producing a nearly solar abundance pattern above mass number 130. By the r-process content of the Galaxy and the average production per event the Galactic merger rate is limited to 4x10^–5/yr (4x10^–4/yr) for a soft (stiff) NS EOS, if NS mergers are the main source of heavy r-nuclei. The production ratio of radioactive ²³²Th to ²³⁸U attains a stable value of 1.64-1.67, which does not exclude NS mergers as potential sources of heavy r-material in the most metal-poor stars.