A redefinition of the symmetry energy expansion that incorporates finite strangeness consistent with SU(3) flavor symmetry and remains valid beyond typical neutron-star central densities.
The equation of state of neutron matter, symmetry energy, and neutron star structure
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abstract
We review the calculation of the equation of state of pure neutron matter using quantum Monte Carlo (QMC) methods. QMC algorithms permit the study of many-body nuclear systems using realistic two- and three-body forces in a nonperturbative framework. We present the results for the equation of state of neutron matter, and focus on the role of three-neutron forces at supranuclear density. We discuss the correlation between the symmetry energy, the neutron star radius and the symmetry energy. We also combine QMC and theoretical models of the three-nucleon interactions, and recent neutron star observations to constrain the value of the symmetry energy and its density dependence.
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Symmetry Energy Expansion with Strange Dense Matter
A redefinition of the symmetry energy expansion that incorporates finite strangeness consistent with SU(3) flavor symmetry and remains valid beyond typical neutron-star central densities.