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| Main Authors: | , |
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| Format: | Preprint |
| Published: |
2023
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2308.00007 |
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Table of 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.