Compact Star of Holographic Nuclear Matter and GW170817. (arXiv:1902.08477v1 [hep-ph])
<a href="http://arxiv.org/find/hep-ph/1/au:+Hirayama_T/0/1/0/all/0/1">Takayuki Hirayama</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Lin_F/0/1/0/all/0/1">Feng-Li Lin</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Luo_L/0/1/0/all/0/1">Ling-Wei Luo</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Zhang_K/0/1/0/all/0/1">Kilar Zhang</a>
We use a holographic model of quantum chromodynamics to extract the equation
of state (EoS) for the cold nuclear matter of moderate baryon density. This
model is based on the Sakai-Sugimoto model in the deconfined Witten’s geometry
with the additional point-like D4-brane instanton configuration as the
holographic baryons. Our EoS takes the following doubly-polytropic form: $
epsilon=2.629 {cal A}^{-0.192} p^{1.192}+0.131 {cal A}^{0.544} p^{0.456}$
with $cal A$ a tunable parameter of order $10^{-1}$, where $epsilon$ and $p$
are the energy density and pressure, respectively. The sound speed satisfies
the causality constraint and breaks the sound barrier. We solve the
Tolman-Oppenheimer-Volkoff equations for the compact stars. We reach the
reasonable compactness for the proper choices of $cal A$. Based on these
configurations we further calculate the tidal deformability of the single and
binary stars. We find our results agree with the inferred values of LIGO/Virgo
data analysis for GW170817.
We use a holographic model of quantum chromodynamics to extract the equation
of state (EoS) for the cold nuclear matter of moderate baryon density. This
model is based on the Sakai-Sugimoto model in the deconfined Witten’s geometry
with the additional point-like D4-brane instanton configuration as the
holographic baryons. Our EoS takes the following doubly-polytropic form: $
epsilon=2.629 {cal A}^{-0.192} p^{1.192}+0.131 {cal A}^{0.544} p^{0.456}$
with $cal A$ a tunable parameter of order $10^{-1}$, where $epsilon$ and $p$
are the energy density and pressure, respectively. The sound speed satisfies
the causality constraint and breaks the sound barrier. We solve the
Tolman-Oppenheimer-Volkoff equations for the compact stars. We reach the
reasonable compactness for the proper choices of $cal A$. Based on these
configurations we further calculate the tidal deformability of the single and
binary stars. We find our results agree with the inferred values of LIGO/Virgo
data analysis for GW170817.
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