Gravitational Waves from Holographic Neutron Star Mergers. (arXiv:1908.03213v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ecker_C/0/1/0/all/0/1">Christian Ecker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jarvinen_M/0/1/0/all/0/1">Matti Järvinen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nijs_G/0/1/0/all/0/1">Govert Nijs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schee_W/0/1/0/all/0/1">Wilke van der Schee</a>
We simulate the merger of binary neutron stars and analyze the spectral
properties of their gravitational waveforms. For the stars we construct hybrid
equations of state (EoSs) with a standard nuclear matter EoS at low densities,
transitioning to a state-of-the-art holographic EoS in the otherwise
intractable high density regime. Depending on the transition density the
characteristic frequencies in the spectrum produced from the hybrid EoSs are
shifted to significantly lower values as compared to the pure nuclear matter
EoS. The highest rest-mass density reached outside a possible black hole
horizon is approximately $1.1 cdot 10^{15}$ g/cm$^3$, which for the
holographic model is below the density of the deconfined quark matter phase.
We simulate the merger of binary neutron stars and analyze the spectral
properties of their gravitational waveforms. For the stars we construct hybrid
equations of state (EoSs) with a standard nuclear matter EoS at low densities,
transitioning to a state-of-the-art holographic EoS in the otherwise
intractable high density regime. Depending on the transition density the
characteristic frequencies in the spectrum produced from the hybrid EoSs are
shifted to significantly lower values as compared to the pure nuclear matter
EoS. The highest rest-mass density reached outside a possible black hole
horizon is approximately $1.1 cdot 10^{15}$ g/cm$^3$, which for the
holographic model is below the density of the deconfined quark matter phase.
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