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Numerical evolutions of boson stars in Palatini $f(\mathcal{R})$ gravity

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arxiv 2309.14912 v1 pith:Q3NUVZ6T submitted 2023-09-26 gr-qc astro-ph.HE

Andreu Masó-Ferrando , Nicolas Sanchis-Gual , José A. Font , Gonzalo J. Olmo This is my paper · ORCID
classification gr-qcastro-ph.HE
keywords mathcalgravityrelativitybosonnumericalpalatinistarsevolutions
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abstract

We investigate the time evolution of spherically symmetric boson stars in Palatini $f(\mathcal{R})$ gravity through Numerical Relativity computations. Employing a novel approach that establishes a correspondence between modified gravity with scalar matter and General Relativity with modified scalar matter, we are able to use the techniques of Numerical Relativity to simulate these systems. Specifically, we focus on the quadratic theory $f(\mathcal{R})=\mathcal{R}+\xi\mathcal{R}^2$ and compare the obtained solutions with those in General Relativity, exploring both positive and negative values of the coupling parameter $\xi$. Our findings reveal that boson stars in Palatini $f(\mathcal{R})$ gravity exhibit both stable and unstable evolutions. The latter give rise to three distinct scenarios: migration towards a stable configuration, complete dispersion, and gravitational collapse leading to the formation of a baby universe structure.

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Cited by 3 Pith papers

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    gr-qc 2025-09 conditional novelty 7.0 of 10

    A fine-tuned Oppenheimer-Snyder collapse with a zero-size initial de-Sitter bubble can end as a static gravastar, with a maximum initial compactness of 3/8.

  2. Rotating Fermion-Boson Stars in $R$-squared Gravity

    gr-qc 2026-07 conditional novelty 6.0 of 10

    R-squared gravity enlarges the equilibrium domain of rotating fermion-boson stars and raises static and Keplerian maximum masses relative to GR while remaining compatible with current compact-object constraints.

  3. Boson Stars in Bumblebee Gravity and Their Gravitational Waveforms from Extreme-Mass-Ratio Inspirals

    gr-qc 2025-12 conditional novelty 5.0 of 10

    In bumblebee gravity, the Lorentz-violating parameter ℓ makes mini-boson stars more compact for positive ℓ and produces LISA-detectable, sustained EMRI waveforms for penetrating orbits.

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