A constrained evolutionary pipeline identifies over 14,000 causal EoS reconciling GW170817 and GW190814 with non-monotonic sound speeds, M_max 2.3-2.8 solar masses, and R_1.4 around 12 km.
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The frequency of global core g-modes in warm neutron stars can be higher or lower than in cold stars depending on the nuclear symmetry energy slope L.
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Reconciling GW170817 and GW190814 with a Nonmonotonic Sound-Speed Equation of State
A constrained evolutionary pipeline identifies over 14,000 causal EoS reconciling GW170817 and GW190814 with non-monotonic sound speeds, M_max 2.3-2.8 solar masses, and R_1.4 around 12 km.
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Finite temperature effects on g-modes of inviscid neutron stars
The frequency of global core g-modes in warm neutron stars can be higher or lower than in cold stars depending on the nuclear symmetry energy slope L.