  The stages that follow the merging of two neutron stars are discussed. It is
shown that if a rapidly rotating gravitationally bound object is formed after
the merging (a spinar or a massive neutron star), then the characteristic time
of its evolution is determined by a fundamental value t_{spin} = 3 k (m_p e^2
\hbar^{1/2}) / (m_e^3 c^{5/2} G^{1/2}) \approx 7e+5 s k, where the
dimensionless value k depends on the exact equation of state of nuclear matter.
The hypothesis is discussed as to whether the residual optical emission of the
gamma-ray burst GRB 970228 is pulsar-like and its evolution driven by
magnetodipole energy losses. It is shown that binary neutron star mergings can
be accompanied by two gravitational wave burst separated either by the time
interval t_{spin} or neutron star cooling time (~10 s), depending on the masses
of neutron stars.
