Constraining the nuclear equation of state from terrestrial experiments and neutron star observations using relativistic mean-field models
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arXiv
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| Autori principali: | , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| _version_ | 1866918254701707264 |
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| author | Miyatsu, Tsuyoshi Cheoun, Myung-Ki Kim, Kyungsik Saito, Koichi |
| author_facet | Miyatsu, Tsuyoshi Cheoun, Myung-Ki Kim, Kyungsik Saito, Koichi |
| contents | We investigate the nuclear equation of state (EoS) for isospin-asymmetric matter using a new set of RMF interactions with the $σ$-$δ$ and $ω$-$ρ$ mixing, referred to as the OMEG family. These interactions are optimized so as to reproduce both terrestrial nuclear measurements and astrophysical constraints extracted from NICER and GW170817. The $σ$-$δ$ mixing softens the nuclear symmetry energy and pressure around twice the saturation density, which enables relatively small neutron-star radii and tidal deformabilities while keeping the nuclear EoS sufficiently stiff at high densities to support $2M_{\odot}$ neutron stars. We find that the curvature parameter, $K_{\textrm{sym}}$, plays an important role in realizing the soft-to-hard behavior of the nuclear EoS, and the astrophysical data favor small or even negative values of $K_{\textrm{sym}}$. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2512_16429 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Constraining the nuclear equation of state from terrestrial experiments and neutron star observations using relativistic mean-field models Miyatsu, Tsuyoshi Cheoun, Myung-Ki Kim, Kyungsik Saito, Koichi Nuclear Theory High Energy Astrophysical Phenomena We investigate the nuclear equation of state (EoS) for isospin-asymmetric matter using a new set of RMF interactions with the $σ$-$δ$ and $ω$-$ρ$ mixing, referred to as the OMEG family. These interactions are optimized so as to reproduce both terrestrial nuclear measurements and astrophysical constraints extracted from NICER and GW170817. The $σ$-$δ$ mixing softens the nuclear symmetry energy and pressure around twice the saturation density, which enables relatively small neutron-star radii and tidal deformabilities while keeping the nuclear EoS sufficiently stiff at high densities to support $2M_{\odot}$ neutron stars. We find that the curvature parameter, $K_{\textrm{sym}}$, plays an important role in realizing the soft-to-hard behavior of the nuclear EoS, and the astrophysical data favor small or even negative values of $K_{\textrm{sym}}$. |
| title | Constraining the nuclear equation of state from terrestrial experiments and neutron star observations using relativistic mean-field models |
| topic | Nuclear Theory High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2512.16429 |