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| Format: | Preprint |
| Published: |
2026
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| Online Access: | https://arxiv.org/abs/2605.14887 |
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| _version_ | 1866918501706366976 |
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| author | Pérez-Garrido, A. |
| author_facet | Pérez-Garrido, A. |
| contents | Brown dwarfs, being transitional objects between giant planets and low-mass stars, possess dense, cool interiors that provide optimal conditions to explore non-standard physics. Capture and accumulation of dark-matter particles can alter the thermal, structural and dynamic of these substellar objects. We aim to apply a self-consistent two-fluid framework to model the internal structure of self-gravitating brown dwarfs and to quantify how the presence of a dark-matter component modifies their mass--radius relations and dynamical properties. The brown dwarf is modeled as a composite system of a baryonic fluid, described by a polytropic equation of state, and an independent dark-matter fluid. Both components are coupled through their shared gravitational potential in hydrostatic equilibrium. We solve numerically the coupled Lane-Emden equations for a range of dark-matter mass fractions. We find that dark matter accumulating in the core reshapes the baryonic density profile, modifying both the radius and the second-order Love number. Radius and dynamical anomalies in brown dwarfs can serve as diagnostic tools to constrain dark-matter properties. Future high-precision astrometric missions could identify these structural signatures, establishing brown dwarfs as possible detectors of dark matter in the Galaxy. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2605_14887 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Self-Interacting Dark Matter in Brown Dwarfs Pérez-Garrido, A. Solar and Stellar Astrophysics Brown dwarfs, being transitional objects between giant planets and low-mass stars, possess dense, cool interiors that provide optimal conditions to explore non-standard physics. Capture and accumulation of dark-matter particles can alter the thermal, structural and dynamic of these substellar objects. We aim to apply a self-consistent two-fluid framework to model the internal structure of self-gravitating brown dwarfs and to quantify how the presence of a dark-matter component modifies their mass--radius relations and dynamical properties. The brown dwarf is modeled as a composite system of a baryonic fluid, described by a polytropic equation of state, and an independent dark-matter fluid. Both components are coupled through their shared gravitational potential in hydrostatic equilibrium. We solve numerically the coupled Lane-Emden equations for a range of dark-matter mass fractions. We find that dark matter accumulating in the core reshapes the baryonic density profile, modifying both the radius and the second-order Love number. Radius and dynamical anomalies in brown dwarfs can serve as diagnostic tools to constrain dark-matter properties. Future high-precision astrometric missions could identify these structural signatures, establishing brown dwarfs as possible detectors of dark matter in the Galaxy. |
| title | Self-Interacting Dark Matter in Brown Dwarfs |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2605.14887 |