Compact Boson Stars
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We consider compact boson stars that arise for a V-shaped scalar field potential. They represent a one parameter family of solutions of the scaled Einstein-signum-Gordon equations. We analyze the physical properties of these solutions and determine their domain of existence. Along their physically relevant branch emerging from the compact Q-ball solution, their mass increases with increasing radius. Empoying arguments from catastrophe theory we argue that this branch is stable, until the maximal value of the mass is reached. There the mass and size are on the order of magnitude of the Schwarzschild limit, and thus the spiralling respectively oscillating behaviour, well-known for compact stars, sets in.
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Forward citations
Cited by 3 Pith papers
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Numerical evolutions of quartically self-interacting boson stars reveal three merger outcomes and a non-monotonic gravitational-wave energy pattern driven by the competition between compactness and tidal deformability.
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Dynamical Boson Stars
Boson stars are particle-like solutions in general relativity that model dark matter, black hole mimickers, and binary systems.
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