Implications of PREX-II on the equation of state of neutron-rich matter. (arXiv:2101.03193v2 [nucl-th] UPDATED)
<a href="http://arxiv.org/find/nucl-th/1/au:+Reed_B/0/1/0/all/0/1">Brendan T. Reed</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Fattoyev_F/0/1/0/all/0/1">F. J. Fattoyev</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Horowitz_C/0/1/0/all/0/1">C. J. Horowitz</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Piekarewicz_J/0/1/0/all/0/1">J. Piekarewicz</a>

Laboratory experiments sensitive to the equation of state of neutron rich
matter in the vicinity of nuclear saturation density provide the first rung in
a “density ladder” that connects terrestrial experiments to astronomical
observations. In this context, the neutron skin thickness of 208Pb (Rskin)
provides the most stringent laboratory constraint on the density dependence of
the symmetry energy. In turn, the cleanest and most precise value of Rskin has
been reported recently by the PREX collaboration. Exploiting the strong
correlation between Rskin and the slope of the symmetry energy (L) we report a
value of L=(106 +/- 37)MeV — that systematically overestimates current limits
based on both theoretical approaches and experimental measurements. The impact
of such a stiff symmetry energy on some critical neutron-star observables is
also examined.

Laboratory experiments sensitive to the equation of state of neutron rich
matter in the vicinity of nuclear saturation density provide the first rung in
a “density ladder” that connects terrestrial experiments to astronomical
observations. In this context, the neutron skin thickness of 208Pb (Rskin)
provides the most stringent laboratory constraint on the density dependence of
the symmetry energy. In turn, the cleanest and most precise value of Rskin has
been reported recently by the PREX collaboration. Exploiting the strong
correlation between Rskin and the slope of the symmetry energy (L) we report a
value of L=(106 +/- 37)MeV — that systematically overestimates current limits
based on both theoretical approaches and experimental measurements. The impact
of such a stiff symmetry energy on some critical neutron-star observables is
also examined.

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