Yuichiro Sekiguchi, Kenta Kiuchi, Koutarou Kyutoku, Masaru Shibata
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 for the first
time. It is found that even for the hyperonic EOS, a hypermassive neutron star
is first formed after the merger for the typical total mass $\approx$
2.7M\bigodot, and subsequently collapses to a black hole (BH). It is shown that
hyperons play a substantial role in the post-merger dynamics, torus formation
around the BH, and emission of gravitational waves (GWs). In particular, the
existence of hyperons is imprinted in GWs. Therefore, GW observations will
provide a potential opportunity to explore the composition of the neutron star
matter.
View original:
http://arxiv.org/abs/1110.4442
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