Dark interactions in neutron star interiors: the interplay of baryons, dark matter, and dark energy
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| Format: | Preprint |
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2025
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| author | Araujo, L. F. Lugones, G. Lima, J. A. S. |
| author_facet | Araujo, L. F. Lugones, G. Lima, J. A. S. |
| contents | The impact of energy exchange among the relevant fluid components: baryonic matter, fermionic dark matter (DM), and dark energy (DE) on the internal structure of neutron stars is investigated. Using a representative DM mass $m_χ = 10$ GeV and a barotropic DE relation, we add source terms Qi to the Tolman-Oppenheimer-Volkoff equations and examine three cases: (i) noninteracting fluids (Model I), (ii) fully interacting baryon plus DM and DM with DE fluids with optional DM self repulsion (Model II), and (iii) a unified dark sector coupled to baryons (Model III). Two effects dominate: softening by massive, pressure-poor DM, and additional softening/ and binding from DE with negative pressures. Model I isolates these baselines. In Model II, exchange terms self regulate, making the mass radius curves nearly independent of the coupling parameter $α$ for nearly five orders of magnitude. Model III breaks this $α$ degeneracy: a sizable vacuum fraction suppresses the baryonic pressure gradient, reducing both the maximum mass and radii, whereas a pure-DM core is less sensitive. We outline when dark interactions can leave observable, macroscopic imprints. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2509_16484 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Dark interactions in neutron star interiors: the interplay of baryons, dark matter, and dark energy Araujo, L. F. Lugones, G. Lima, J. A. S. High Energy Astrophysical Phenomena High Energy Physics - Phenomenology The impact of energy exchange among the relevant fluid components: baryonic matter, fermionic dark matter (DM), and dark energy (DE) on the internal structure of neutron stars is investigated. Using a representative DM mass $m_χ = 10$ GeV and a barotropic DE relation, we add source terms Qi to the Tolman-Oppenheimer-Volkoff equations and examine three cases: (i) noninteracting fluids (Model I), (ii) fully interacting baryon plus DM and DM with DE fluids with optional DM self repulsion (Model II), and (iii) a unified dark sector coupled to baryons (Model III). Two effects dominate: softening by massive, pressure-poor DM, and additional softening/ and binding from DE with negative pressures. Model I isolates these baselines. In Model II, exchange terms self regulate, making the mass radius curves nearly independent of the coupling parameter $α$ for nearly five orders of magnitude. Model III breaks this $α$ degeneracy: a sizable vacuum fraction suppresses the baryonic pressure gradient, reducing both the maximum mass and radii, whereas a pure-DM core is less sensitive. We outline when dark interactions can leave observable, macroscopic imprints. |
| title | Dark interactions in neutron star interiors: the interplay of baryons, dark matter, and dark energy |
| topic | High Energy Astrophysical Phenomena High Energy Physics - Phenomenology |
| url | https://arxiv.org/abs/2509.16484 |