Neutron stars in $f(\mathbb{Q})$ gravity
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arXiv
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| Format: | Preprint |
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2025
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| author | Heisenberg, Lavinia Pastor-Marcos, Carlos |
| author_facet | Heisenberg, Lavinia Pastor-Marcos, Carlos |
| contents | We investigate the challenges of constructing neutron star (NS) solutions in $f(\mathbb{Q})$ gravity, highlighting the importance of treating the affine connection as an active, dynamical component of the theory. We begin by clarifying under what conditions standard simplifications -- such as the coincident gauge or General Relativity (GR)-like connections -- inadvertently lead to GR behavior, even in non-trivial $f(\mathbb{Q})$ models. Building on previous work in black hole (BH) spacetimes, we adapt the formalism to NS and extend it to non-vacuum configurations. Focusing on two representative models, $f(\mathbb{Q}) = \mathbb{Q} + α\mathbb{Q}^2$ and $f(\mathbb{Q}) = \mathbb{Q}^β$, our analysis suggests that, under standard regularity assumptions, solutions with Maclaurin/Laurent-type series recover GR dynamics, pointing to more intricate structures as the likely seat of beyond-GR effects, and reflecting the constraints imposed by the connection's dynamics on the asymptotic behavior of genuinely beyond-GR solutions. We then formulate the problem as a boundary value problem (BVP) and highlight the numerical pathologies that may arise, together with possible strategies to prevent them. This work aims to provide a concrete framework for future numerical studies and outlines the theoretical consistency conditions required to construct physically meaningful beyond-GR NS solutions in $f(\mathbb{Q})$ gravity. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2512_03037 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Neutron stars in $f(\mathbb{Q})$ gravity Heisenberg, Lavinia Pastor-Marcos, Carlos General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena We investigate the challenges of constructing neutron star (NS) solutions in $f(\mathbb{Q})$ gravity, highlighting the importance of treating the affine connection as an active, dynamical component of the theory. We begin by clarifying under what conditions standard simplifications -- such as the coincident gauge or General Relativity (GR)-like connections -- inadvertently lead to GR behavior, even in non-trivial $f(\mathbb{Q})$ models. Building on previous work in black hole (BH) spacetimes, we adapt the formalism to NS and extend it to non-vacuum configurations. Focusing on two representative models, $f(\mathbb{Q}) = \mathbb{Q} + α\mathbb{Q}^2$ and $f(\mathbb{Q}) = \mathbb{Q}^β$, our analysis suggests that, under standard regularity assumptions, solutions with Maclaurin/Laurent-type series recover GR dynamics, pointing to more intricate structures as the likely seat of beyond-GR effects, and reflecting the constraints imposed by the connection's dynamics on the asymptotic behavior of genuinely beyond-GR solutions. We then formulate the problem as a boundary value problem (BVP) and highlight the numerical pathologies that may arise, together with possible strategies to prevent them. This work aims to provide a concrete framework for future numerical studies and outlines the theoretical consistency conditions required to construct physically meaningful beyond-GR NS solutions in $f(\mathbb{Q})$ gravity. |
| title | Neutron stars in $f(\mathbb{Q})$ gravity |
| topic | General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2512.03037 |