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PreprintarXiv licencearXiv

Higher-Order Symmetry Energy Effects on the Properties of Neutron Stars

  • Zijing Zhou
  • Xuhao Wu
  • Shishao Bao
  • Min Ju
  • Jinniu Hu
  • Hong Shen
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Abstract

We study the effects of the symmetry-energy curvature Ksym on the equation of state (EoS) and neutron-star properties within the relativistic mean-field (RMF) framework. We construct controlled families of RMF parametrizations based on the TM1 and IUFSU models by varying Ksym while keeping the symmetry energy J and its slope L fixed at saturation density. We find that, although a larger Ksym leads to a lower symmetry energy at suprasaturation densities and a reduced proton fraction in β-equilibrated matter, it results in a stiffer EoS and a higher sound speed. The maximum neutron-star mass is weakly affected, whereas the canonical radius R1.4 exhibits a nearly linear dependence on Ksym.

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Cite

BibTeXRIS
BibTeX
@misc{zhou2026higherorder,
  title = {{Higher-Order Symmetry Energy Effects on the Properties of Neutron Stars}},
  author = {Zijing Zhou and Xuhao Wu and Shishao Bao and Min Ju and Jinniu Hu and Hong Shen},
  howpublished = {arXiv},
  year = {2026},
  month = nov,
  doi = {10.48550/arxiv.2611.01722},
  eprint = {2611.01722},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2611.01722},
}
RIS
TY  - UNPB
TI  - Higher-Order Symmetry Energy Effects on the Properties of Neutron Stars
AU  - Zijing Zhou
AU  - Xuhao Wu
AU  - Shishao Bao
AU  - Min Ju
AU  - Jinniu Hu
AU  - Hong Shen
PY  - 2026
DA  - 2026/11/01
PB  - arXiv
DO  - 10.48550/arxiv.2611.01722
UR  - https://arxiv.org/abs/2611.01722
AB  - We study the effects of the symmetry-energy curvature K_sym on the equation of state (EoS) and neutron-star properties within the relativistic mean-field (RMF) framework. We construct controlled families of RMF parametrizations based on the TM1 and IUFSU models by varying K_sym while keeping the symmetry energy J and its slope L fixed at saturation density. We find that, although a larger K_sym leads to a lower symmetry energy at suprasaturation densities and a reduced proton fraction in β-equilibrated matter, it results in a stiffer EoS and a higher sound speed. The maximum neutron-star mass is weakly affected, whereas the canonical radius R_1.4 exhibits a nearly linear dependence on K_sym.
ER  -