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 _ { life } \gtrsim 10 ~ { } { 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 _ { life } \approx 3 ~ { } { 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 } ~ { } { erg / s } and the effective amplitude of gravitational waves from the HMNS is 1 – 4 \times 10 ^ { -22 } at f \approx 2 – 3.2 ~ { } { 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 .