Parity-doubled nucleons can rapidly cool neutron stars
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arXiv
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| Format: | Preprint |
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2025
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| _version_ | 1866915570458296320 |
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| author | Brodie, Liam Pisarski, Robert D. |
| author_facet | Brodie, Liam Pisarski, Robert D. |
| contents | In confined hadronic matter, the spontaneous breaking and restoration of chiral symmetry can be described by considering nucleons, $N_{+}(939)$, and excited states of opposite parity, $N_{-}(1535)$. In a cold, dense hadronic phase where chiral symmetry remains spontaneously broken, direct Urca decay processes involving the $N_{-}$ are possible, e.g. $N_- \rightarrow N_+ + e^- + \barν_e$. We show that at low temperature and moderate densities, because the $N_-$ is much heavier than the $N_+$, such cooling dominates over standard $N_+$ direct Urca processes. This provides a strong astrophysical signature of the pattern of chiral symmetry restoration in neutron stars. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2501_02055 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Parity-doubled nucleons can rapidly cool neutron stars Brodie, Liam Pisarski, Robert D. Nuclear Theory High Energy Astrophysical Phenomena High Energy Physics - Phenomenology In confined hadronic matter, the spontaneous breaking and restoration of chiral symmetry can be described by considering nucleons, $N_{+}(939)$, and excited states of opposite parity, $N_{-}(1535)$. In a cold, dense hadronic phase where chiral symmetry remains spontaneously broken, direct Urca decay processes involving the $N_{-}$ are possible, e.g. $N_- \rightarrow N_+ + e^- + \barν_e$. We show that at low temperature and moderate densities, because the $N_-$ is much heavier than the $N_+$, such cooling dominates over standard $N_+$ direct Urca processes. This provides a strong astrophysical signature of the pattern of chiral symmetry restoration in neutron stars. |
| title | Parity-doubled nucleons can rapidly cool neutron stars |
| topic | Nuclear Theory High Energy Astrophysical Phenomena High Energy Physics - Phenomenology |
| url | https://arxiv.org/abs/2501.02055 |