  Numerical simulations for the merger of binary neutron stars are performed in
full general relativity incorporating both nucleonic and hyperonic
finite-temperature equations of state (EOS) and neutrino cooling. It is found
that for the nucleonic and hyperonic EOS, a hyper massive neutron star (HMNS)
with a long lifetime $(t_{\rm life}\gtrsim 10 {\rm ms})$ is the outcome for the
total mass $\approx 2.7 M_\odot$. For the total mass $\approx 3 M_\odot$, a
long-lived (short-lived with $t_{\rm life}\approx 3 {\rm ms}$) HMNS is the
outcome for the nucleonic (hyperonic) EOS. It is shown that the typical total
neutrino luminosity of the HMNS is $\sim 3$ -- $6 \times 10^{53} {\rm erg /s}$
and the effective amplitude of gravitational waves from the HMNS is 1 --
$4\times 10^{-22}$ at $f\approx 2$ -- $3.2 {\rm kHz}$ for a source of distance
of 100 Mpc. During the HMNS phase, characteristic frequencies of gravitational
waves shift to a higher frequency for the hyperonic EOS in contrast to the
nucleonic EOS in which they remain constant approximately. Our finding suggests
that the effects of hyperons are well imprinted in gravitational wave and its
detection will give us a potential opportunity to explore the composition of
the neutron star matter. We present the neutrino luminosity curve when a black
hole is formed as well.
