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| Natura: | Preprint |
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2023
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| Accesso online: | https://arxiv.org/abs/2308.00007 |
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| _version_ | 1866908595753320448 |
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| author | Wu, Chen Guo, Wenjun |
| author_facet | Wu, Chen Guo, Wenjun |
| contents | In this work, we study the properties of neutron stars using the linear Relativistic Mean-Field (RMF) theory and consider multiple degrees of freedom inside neutron stars, including hyperons and $Δ$ resonances. We investigate different coupling parameters $x_{σΔ}$ between $Δ$ resonances and nucleons and compare the differences between neutron stars with and without strange mesons $σ^*$ and $ϕ$. These effects include particle number distributions, equations of state (EOS), mass-radius relations, and tidal deformabilities. To overcome the "hyperon puzzle," we employ the $σ-cut$ scheme to obtain neutron stars with masses up to $2M_{\odot}$. We find that strange mesons appear at around 3$ρ_0$ and reduce the critical density of baryons in the high-density region. With increasing coupling parameter $x_{σΔ}$, the $Δ$ resonances suppress hyperons, leading to a shift of the critical density towards lower values. The early appearance of $Δ$ resonances may play a crucial role in the stability of neutron stars. Strange mesons soften the EOS slightly, while $Δ$ resonances predominantly soften the EOS in the low-density region. By calculating tidal deformabilities and comparing with astronomical observation GW170817, we find that the inclusion of $Δ$ resonances decreases the radius of neutron stars. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2308_00007 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Effects of Phi and $σ^{*}$-meson on properties of hyperon stars including $Δ$ resonance Wu, Chen Guo, Wenjun Nuclear Theory High Energy Astrophysical Phenomena In this work, we study the properties of neutron stars using the linear Relativistic Mean-Field (RMF) theory and consider multiple degrees of freedom inside neutron stars, including hyperons and $Δ$ resonances. We investigate different coupling parameters $x_{σΔ}$ between $Δ$ resonances and nucleons and compare the differences between neutron stars with and without strange mesons $σ^*$ and $ϕ$. These effects include particle number distributions, equations of state (EOS), mass-radius relations, and tidal deformabilities. To overcome the "hyperon puzzle," we employ the $σ-cut$ scheme to obtain neutron stars with masses up to $2M_{\odot}$. We find that strange mesons appear at around 3$ρ_0$ and reduce the critical density of baryons in the high-density region. With increasing coupling parameter $x_{σΔ}$, the $Δ$ resonances suppress hyperons, leading to a shift of the critical density towards lower values. The early appearance of $Δ$ resonances may play a crucial role in the stability of neutron stars. Strange mesons soften the EOS slightly, while $Δ$ resonances predominantly soften the EOS in the low-density region. By calculating tidal deformabilities and comparing with astronomical observation GW170817, we find that the inclusion of $Δ$ resonances decreases the radius of neutron stars. |
| title | Effects of Phi and $σ^{*}$-meson on properties of hyperon stars including $Δ$ resonance |
| topic | Nuclear Theory High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2308.00007 |