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Effects of hyperons in binary neutron star mergers
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abstract
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.
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Cited by 1 Pith paper
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Hyperonic degrees of freedom in binary neutron star mergers
A review of neutron star merger simulations showing that hyperonic equations of state yield distinctive gravitational wave, temperature, ejecta, and collapse-threshold signatures.
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