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   https://doi.org/10.1103/PhysRevLett.129.061103  

   Goldman, Itzhak ; Mohapatra, Rabindra N. ; Nussinov, Shmuel ; Zhang, Yongchao ( August 2022 , Physical Review Letters)
2. Neutron-Star Radius from a Population of Binary Neutron Star Mergers

   https://doi.org/10.1103/PhysRevLett.120.031102  

   Bose, Sukanta ; Chakravarti, Kabir ; Rezzolla, Luciano ; Sathyaprakash, B. S. ; Takami, Kentaro ( January 2018 , Physical Review Letters)
3. Inferring Small Neutron Star Spins with Neutron Star–Black Hole Mergers

   https://doi.org/10.3847/1538-4357/ad49a0  

   Gupta, Ish ( July 2024 , The Astrophysical Journal)

   The precise measurement of neutron star (NS) spins can provide important insight into the formation and evolution of compact binaries containing NSs. While traditional methods of NS spin measurement rely on pulsar observations, gravitational-wave detections offer a complementary avenue. However, determining component spins with gravitational waves is hindered by the small dimensionless spins of the NSs and the degeneracy in the mass and spin parameters. This degeneracy can be addressed by the inclusion of higher-order modes in the waveform, which are important for systems with unequal masses. This study shows the suitability of NS–black hole mergers, which are naturally mass-asymmetric, for precise NS spin measurements. We explore the effects of the black hole masses and spins, higher-mode content, inclination angles, and detector sensitivity on the measurement of NS spin. We find that networks with next-generation observatories like the Cosmic Explorer and the Einstein Telescope can distinguish NS dimensionless spin of 0.04 (0.1) from zero at 1σconfidence for events within ∼350 (∼1000) Mpc. Networks with A+ and A^♯detectors achieve similar distinction within ∼30 (∼70) Mpc and ∼50 (∼110) Mpc, respectively.

    

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4. Gravitational waveforms from spectral Einstein code simulations: Neutron star-neutron star and low-mass black hole-neutron star binaries

   https://doi.org/10.1103/PhysRevD.99.044008  

   Foucart, F. ; Duez, M. D. ; Hinderer, T. ; Caro, J. ; Williamson, Andrew R. ; Boyle, M. ; Buonanno, A. ; Haas, R. ; Hemberger, D. A. ; Kidder, L. E. ; et al ( February 2019 , Physical Review D)
5. Proto-Neutron Star Matter

   https://doi.org/10.1088/1742-6596/2340/1/012013  

   Alp, A ; Farrell, D ; Weber, F ; Malfatti, G ; Orsaria, M G ; Ranea-Sandoval, I F ( September 2022 , Journal of Physics: Conference Series)

   Abstract In this paper, we explore the properties of proto-neutron star matter. The relativistic finite-temperature Green function formalism is used to derive the equations which determine the properties of such matter. The calculations are performed for the relativistic non-linear mean-filed theory, where different combinations of lepton number and entropy have been investigated. All particles of the baryon octet as well as all electrically charged states of the Δ isobar have been included in the calculations. The presence of all these particles is shown to be extremely temperature (entropy) dependent, which should have important consequences for the evolution of proto-neutron stars to neutron stars as well as the behavior of neutron stars in compact star mergers. 

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