Coalescing neutron stars -- a step towards physical models. II. Neutrino emission, neutron tori, and gamma-ray bursts

Abstract

Three-dimensional hydrodynamical, Newtonian calculations of the coalescence of equal-mass binary neutron stars are performed, including a physical high-density equation of state and a treatment of the neutrino emission of the heated matter. The total neutrino luminosity climbs to a maximum value of 1--$1.5\cdot 10^{53}$~erg/s of which 90--95\% originate from the toroidal gas cloud surrounding the very dense core formed after the merging. When the neutrino luminosities are highest, $\hat{I}½\bar{\hat{I}}½$-annihilation deposits about 0.2--0.3\% of the emitted neutrino energy in the immediate neighborhood of the merger, and the maximum integral energy deposition rate is 3--$4\cdot 10^{50}$~erg/s. Since the $3M_{\odot }$ core of the merged object will most likely collapse into a black hole within milliseconds, the energy that can be pumped into a pair-photon fireball is insufficient by a factor of about 1000 to explain ${\hat{I}}^3$-ray bursts at cosmological distances with an energy of the order of $10^{51}/(4\ddot{I}€)$~erg/steradian. Analytical estimates show that the additional energy provided by the annihilation of $\hat{I}½\bar{\hat{I}}½$ pairs emitted from a possible accretion torus of $\sim 0.1M_{\odot }$ around the central black hole is still more than a factor of 10 too small, unless focussing of the fireball into a jet-like expansion plays an important role. About $10^{-4}$--$10^{-3}$~$M_{\odot }$ of material lost during the neutron star merging and swept out from the system in a neutrino-driven wind might be a site for nucleosythesis. Aspects of a possible r-processing in these ejecta are discussed.

35 pages including some figures. Missing figures can be obtained from the authors. Submitted to A&A