-
[1]
Y. Suwa, From supernovae to neutron stars, Publ. Astron. Soc. Jpn. 66 (2014) L1
-
[2]
M. Oertel, M. Hempel, and T. Klähn, and S. Typel, Equations of state for supernovae and compact stars, Rev. Mod. Phys. 89 (2017) 015007. doi:10.1103/RevModPhys.89.015007.
-
[3]
H. Shen, H. Toki, K. Oyamatsu, and K. Sumiyoshi, Relativistic Equation of State of Nuclear Matter for Supernova Explosion, Prog. Theor. Phys. 100 (1998) 1013-1031. doi:10.1143/PTP.100.1013.
-
[4]
T. Yamasaki and S. Yamada, Standing Accretion Shocks in the Supernova Core: Effects of Convection and Realistic Equations of State, Astrophys. J. 887 (2006) L21. doi:10.1086/507067.
-
[5]
C. Constantinou, B. Muccioli, M. Prakash, and J. M. Lattimer, Thermal properties of supernova matter: The bulk homogeneous phase, Phys. Rev. C 89 (2014) 065802. doi:10.1103/PhysRevC.89.065802.
-
[6]
Q. A. Mabanta and J. W. Murphy, How Turbulence Enables Core-collapse Supernova Explosions, Astrophys. J. 856 (2018) 22. doi:10.3847/1538-4357/aaaec7.
-
[7]
A. Burrows T. Wang and D. Vartanyan, Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory, Astrophys. J. Lett. 964 (2024) L16. doi:10.3847/2041-8213/ad319e.
-
[8]
M. Prakash, J. M. Lattimer, J. A. Pons, A. W. Steiner, and S. Reddy, Evolution of a Neutron Star from Its Birth to Old Age, Lect. Notes Phys. 578 (2001) 364–423. doi:10.1007/3-540-44578-1_14.
-
[9]
G.-Y. Shao, Evolution of proto-neutron stars with the hadron-quark phase transition, Phys. Lett. B 704 (2011) 343-346. doi:10.1016/j.physletb.2011.09.030.
-
[10]
P.-C. Chu, and L.-W. Chen, Warm asymmetric quark matter and protoquark stars within the confined isospin-density-dependent mass model, Phys. Rev. D 96 (2017) 103001. doi:10.1103/PhysRevD.96.103001.
-
[11]
A. R Raduta, M. Oertel, and A. Sedrakian, Proto-neutron stars with heavy baryons and universal relations, Mon. Not. R. Astron. Soc. 499 (2020) 914-931. doi:10.1093/mnras/staa2491.
-
[12]
K. Sumiyoshi, S. Furusawa, H. Nagakura, A. Harada, H. Togashi, K. Nakazato, and H. Suzuki, Effects of nuclear matter and composition in core-collapse supernovae and long-term proto-neutron star cooling, Prog. Theor. Exp. Phys. 2023 (2022) 013E02. doi:10.1093/ptep/ptac167.
-
[13]
P.-C. Chu, H. Liu, M. Ju, X.-H. Wu, H.-M. Liu, Y. Zhou, H. Liu, S.-Y. Lu, and X.-H. Li, Quark star matter in color-flavor-locked phase at finite temperature, Phys. Rev. D 110 (2024) 043032. doi:10.1103/PhysRevD.110.043032.
-
[14]
M. Shibata and K. Taniguchi, Coalescence of Black Hole-Neutron Star Binaries, Living Rev. Relativity 14 (2011) 6. doi:10.12942/lrr-2011-6.
-
[15]
M. Ruiz, A. Tsokaros, and S. L. Shapiro, Magnetohydrodynamic simulations of binary neutron star mergers in general relativity: Effects of magnetic field orientation on jet launching, Phys. Rev. D 101 (2020) 064042. doi:10.1103/PhysRevD.101.064042.
-
[16]
S. Li and J. Pang and H. Shen and J. N. Hu and K. Sumiyoshi, Influence of effective nucleon mass on equation of state for supernova simulations and neutron stars, arXiv: 2407.18739.
-
[17]
C. Ducoin, J. Margueron and C. Providência, Nuclear symmetry energy and core-crust transition in neutron stars: A critical study, Europhys. Lett. 91 (2010) 32001. doi:10.1209/0295-5075/91/32001.
-
[18]
R. Cavagnoli, D. P. Menezes, C. Providência, D. P. Menezes, Neutron star properties and the symmetry energy, Phys. Rev. C 86 (2011) 065810. doi:10.1103/PhysRevC.84.065810.
-
[19]
C. Providência, and A. Rabhi, Interplay between the symmetry energy and the strangeness content of neutron stars, Phys. Rev. C 87 (2011) 055801. doi:10.1103/PhysRevC.87.055801.
-
[20]
C. Wellenhofer, J. W. Holt, and N. Kaiser, Thermodynamics of isospin-asymmetric nuclear matter from chiral effective field theory, Phys. Rev. C 92 (2015) 015801. doi:10.1103/PhysRevC.92.015801.
-
[21]
K. Nakazato and H. Suzuki, Cooling Timescale for Protoneutron Stars and Properties of Nuclear Matter: Effective Mass and Symmetry Energy at High Densities, Astrophys. J. 878 (2019) 25. doi:10.3847/1538-4357/ab1d4b.
-
[22]
K. Sumiyoshi, K. Nakazato, H. Suzuki, J. N. Hu and H. Shen, Influence of Density Dependence of Symmetry Energy in Hot and Dense Matter for Supernova Simulations, Astrophys. J. 887 (2019) 110. doi:10.3847/1538-4357/ab5443.
-
[23]
S. S. Bao, J. N. Hu, Z. W. Zhang, and H. Shen, Effects of the symmetry energy on properties of neutron star crusts near the neutron drip density, Phys. Rev. C 90 (2014) 045802. doi:10.1103/PhysRevC.90.045802.
-
[24]
H. Shen and F. Ji and J. N. Hu and K. Sumiyoshi, Influence of Density Dependence of Symmetry Energy in Hot and Dense Matter for Supernova Simulations, Astrophys. J. 891 (2020) 148. doi:10.3847/1538-4357/ab72fd.
-
[25]
Y. Sugahara and H. Toki, Relativistic mean-field theory for unstable nuclei with non-linear σ and ω terms, Nucl. Phys. A 579 (2020) 557-572. doi:10.1016/0375-9474(94)90923-7.
-
[26]
H. Shen, H. Toki, K. Oyamatsu and K. Sumiyoshi, Relativistic Equation of State for Core-Collapse Supernova Simulations, Astrophys. J. Suppl. Ser. 197 (2011) 20. doi:10.1088/0067-0049/197/2/20.
-
[27]
J. Meng, H. Toki, S. G. Zhou, S. Q. Zhang, W. H. Long, and L. S. Geng, Relativistic Continuum Hartree Bogoliubov theory for ground state properties of exotic nuclei, Prog. Part. Nucl. Phys. 57 (2006) 470-563. doi:10.1016/j.ppnp.2005.06.001.
-
[28]
S. S. Bao, and H. Shen, Effects of finite size and symmetry energy on the phase transition of stellar matter at subnuclear densities, Phys. Rev. C 93 (2016) 025807. doi:10.1103/PhysRevC.93.025807.
-
[29]
A. W. Steiner, M. Prakash and J.M. Lattimer, Quark-hadron phase transitions in Young and old neutron stars, Phys. Lett. B 486 (2000) 239-248. doi:10.1016/S0370-2693(00)00780-2.
-
[30]
D. P. Menezes, A. Deppman, E. Megıas, and L. B. Castro, Non-extensive thermodynamics and neutron star properties, Eur. Phys. J. A 51 (2000) 155. doi:10.1140/epja/i2015-15155-3.
-
[31]
P.-C. Chu, B. Wang, Y.-Y Jia, Y.-M. Dong, S.-M. Wang, X.-H. Li, L. Zhang, X. M. Zhang, and H. Y. Ma, Quark magnetar in three-flavor Nambu–Jona-Lasinio model under strong magnetic fields with two types of vector interactions, Phys. Rev. D 94 (2016) 123014. doi:10.1103/PhysRevD.94.123014.
-
[32]
P. Haensel, J. L. Zdunik, and F. Douchin, Equation of state of dense matter and the minimum mass of cold neutron stars, A&A 385 (2002) 301-307. doi:10.1051/0004-6361:20020131.
-
[33]
Y. Suwa, T. Yoshida, M. Shibata, H. Umeda, and K. Takahashi On the minimum mass of neutron stars, Mon. Not. R. Astron. Soc. 481 (2018) 3305-3312. doi:10.1093/mnras/sty2460.
-
[34]
P. S. Koliogiannis and Ch. C. Moustakidis, Thermodynamical Description of Hot, Rapidly Rotating Neutron Stars, Protoneutron Stars, and Neutron Star Merger Remnants, Astrophys. J. 912 (2021) 69. doi:10.3847/1538-4357/abe542.
-
[35]
S. S. Bao, and H. Shen, Impact of the symmetry energy on nuclear pasta phases and crust-core transition in neutron stars, Phys. Rev. C 91 (2015) 015807. doi:10.1103/PhysRevC.91.015807.