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Effect of the symmetry energy and hyperon interaction on neutron stars
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abstract
The joint effect of the density dependence of the symmetry energy and strangeness content on the structure of cold neutron stars is studied within the framework of a relativistic mean field theory. It is shown that 2$M_\odot$ are obtained for repulsive $YY$ interaction and preferably for a small or a large slope $L$. An attractive $\Sigma$ potential in nuclear matter will favor the appearance of strangeness in stars with a mass as small as $\sim 1 M_\odot$, if, however it is repulsive only stars with a mass $\gtrsim 1.4 M_\odot$ will contain strangeness. The joint effect of reducing the symmetry energy slope and including hyperons is to farther reduce the radius. Neutron star maximum mass evolve non-monotonically with the symmetry energy slope, and the smallest masses are obtained for values $L\sim 80$ MeV. Other neutron star variables evolve nonlinearly with the slope of the symmetry energy and depend on the hyperon-nucleon and hyperon-hyperon couplings. The radius of a neutron star is linearly correlated with the neutron star total strangeness fraction and the slope is independent of the slope of the symmetry energy and the mass of the star.
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Cited by 1 Pith paper
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High density symmetry energy: A key to the solution of the hyperon puzzle
A soft-then-stiff symmetry energy delays hyperon appearance and lets hyperon stars reach about 2 solar masses while matching a wide set of astrophysical constraints.
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