The Equation of State of Dense Matter in the Multimessenger Era. (arXiv:1901.11364v1 [nucl-th])
<a href="http://arxiv.org/find/nucl-th/1/au:+Zhou_Y/0/1/0/all/0/1">Ying Zhou</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Chen_L/0/1/0/all/0/1">Lie-Wen Chen</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Zhang_Z/0/1/0/all/0/1">Zhen Zhang</a>

While the equation of state (EOS) of symmetric nuclear matter (SNM) at
suprasaturation densities has been relatively well constrained from heavy-ion
collisions, the EOS of high-density neutron-rich matter is still largely
uncertain due to the poorly known high-density behavior of the symmetry energy.
Using the constraints on the EOS of SNM at suprasaturation densities from
heavy-ion collisions together with the data of finite nuclei and the existence
of $2M_odot$ neutron stars from electromagnetic (EM) observations, we show
that the high-density symmetry energy cannot be too soft, which leads to lower
bounds on dimensionless tidal deformability of $Lambda_{1.4} ge 193$ and
radius of $R_{1.4} ge 11.1$ km for $1.4M_odot$ neutron star. Furthermore, we
find that the recent constraint of $Lambda_{1.4} le 580$ from the
gravitational wave signal GW170817 detected from the binary neutron star merger
by the LIGO and Virgo Collaborations rules out too stiff high-density symmetry
energy, leading to an upper limit of $R_{1.4} le 13.3$ km. All these
terrestrial nuclear experiments and astrophysical observations based on strong,
EM and gravitational measurements together put stringent constraints on the
high-density symmetry energy and the EOS of SNM, pure neutron matter and
neutron star matter.

While the equation of state (EOS) of symmetric nuclear matter (SNM) at
suprasaturation densities has been relatively well constrained from heavy-ion
collisions, the EOS of high-density neutron-rich matter is still largely
uncertain due to the poorly known high-density behavior of the symmetry energy.
Using the constraints on the EOS of SNM at suprasaturation densities from
heavy-ion collisions together with the data of finite nuclei and the existence
of $2M_odot$ neutron stars from electromagnetic (EM) observations, we show
that the high-density symmetry energy cannot be too soft, which leads to lower
bounds on dimensionless tidal deformability of $Lambda_{1.4} ge 193$ and
radius of $R_{1.4} ge 11.1$ km for $1.4M_odot$ neutron star. Furthermore, we
find that the recent constraint of $Lambda_{1.4} le 580$ from the
gravitational wave signal GW170817 detected from the binary neutron star merger
by the LIGO and Virgo Collaborations rules out too stiff high-density symmetry
energy, leading to an upper limit of $R_{1.4} le 13.3$ km. All these
terrestrial nuclear experiments and astrophysical observations based on strong,
EM and gravitational measurements together put stringent constraints on the
high-density symmetry energy and the EOS of SNM, pure neutron matter and
neutron star matter.

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