The lifetime of binary neutron star merger remnants. (arXiv:1909.08631v1 [astro-ph.HE])

The lifetime of binary neutron star merger remnants. (arXiv:1909.08631v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lucca_M/0/1/0/all/0/1">Matteo Lucca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sagunski_L/0/1/0/all/0/1">Laura Sagunski</a>

Although the main features of the evolution of binary neutron star systems
are now well established, many details are still subject to debate, especially
regarding the post-merger phase. In particular, the lifetime of the hyper
massive neutron stars formed after the merger is very hard to predict. In this
work, we provide a simple analytic relation for the lifetime of the merger
remnant as function of the initial mass of the neutron stars. This relation
results from a joint fit of data from observational evidence and from various
numerical simulations. In this way, a large range of collapse times, physical
effects and equation of states is covered. Finally, we apply the relation to
the gravitational wave event GW170817 to constrain the equation of state of
dense matter.

Although the main features of the evolution of binary neutron star systems
are now well established, many details are still subject to debate, especially
regarding the post-merger phase. In particular, the lifetime of the hyper
massive neutron stars formed after the merger is very hard to predict. In this
work, we provide a simple analytic relation for the lifetime of the merger
remnant as function of the initial mass of the neutron stars. This relation
results from a joint fit of data from observational evidence and from various
numerical simulations. In this way, a large range of collapse times, physical
effects and equation of states is covered. Finally, we apply the relation to
the gravitational wave event GW170817 to constrain the equation of state of
dense matter.

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