FORMATION OF A GRAVITATIONALLY BOUND OBJECT AFTER BINARY NEUTRON-STARMERGING AND GRB PHENOMENA

The stages that follow the merging of two neutron stars are discussed. It is shown that if a rapidly rotating gravitationally bound object i s formed after the merging (a spinar or a massive neutron star), then the characteristic time of its evolution is determined by a fundamenta l value t(spin) = 3k . m(p)e(2)h(1/2)/m(e)(3)c(5/2)G(1/2) approximate to 10(3) s.kappa, where the dimensionless value kappa = 100 divided by 1000 depends on the exact equation of state of nuclear matter. The hy pothesis is discussed as to whether the residual optical emission of t he a-ray bursts is pulsar-like and its evolution driven by magnetodipo le energy losses. It is shown that binary neutron star mergings can be accompanied by two gravitational wave burst separated either by the t ime of spinar's collapse t(spin) or neutron star cooling time (similar to 10 s), depending on the masses of neutron stars.