For 1.4 solar mass neutron stars the radius-deformability relation is nearly independent of higher-order nuclear parameters but strongly depends on the symmetry energy slope L, and the relation fails for 1.8 solar mass stars.
Nuclear Astrophysics in the New Era of Multimessenger Astronomy
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Neutron stars are unique cosmic laboratories for the exploration of matter under extreme conditions of density and neutron-proton asymmetry. Due to their enormous dynamic range, neutron stars display a myriad of exotic states of matter that are impossible to recreate under normal laboratory conditions. In these three lectures I will discuss how the strong synergy that has developed between nuclear physics and astrophysics will uncover some of the deepest secrets behind these fascinating objects. In particular, I will highlight the enormous impact that the very first detection of gravitational waves from the binary neutron-star merger GW170817 is having in constraining the composition, structure, and dynamics of neutron stars.
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The key factor to determine the relation between radius and tidal deformability of neutron stars: slope of symmetry energy
For 1.4 solar mass neutron stars the radius-deformability relation is nearly independent of higher-order nuclear parameters but strongly depends on the symmetry energy slope L, and the relation fails for 1.8 solar mass stars.