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.
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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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.