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Dynamical evolution of fermion-boson stars with realistic equations of state
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Fermion-boson stars are mixtures of the ordinary nuclear matter of a neutron star and bosonic dark matter. We dynamically evolve fermion-boson stars for the first time using a realistic equation of state for nuclear matter. We use our dynamical solutions to make a detailed study of the evolution of weakly and strongly perturbed static solutions. As examples of our findings, we identify a region of parameter space where weakly perturbed unstable static solutions migrate to a stable configuration and we determine the criteria under which strongly perturbed stable static solutions will always move to a stable configuration instead of collapsing to a black hole.
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Cited by 3 Pith papers
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Radial spectra and dynamical signatures of excited boson stars
For excited boson stars, the first zero of the fundamental radial mode matches the first critical point of mass, charge, and binding energy for all tested node numbers and self-interactions.
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Rotating Fermion-Boson Stars in $R$-squared Gravity
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.
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Testing bosonic dark matter through white dwarf mass measurements
Adding a bosonic dark-matter core to white dwarf models reproduces the observed electromagnetic-vs-redshift mass discrepancies and the data favor a boson mass near 10^-10 eV.
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