Quartically self-interacting massive boson stars are stable only up to the first mass maximum; their head-on mergers yield a boson-star remnant, a black hole at contact, or two black holes formed before contact, with radiated energy varying non-monotonically at strong coupling.
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Numerical simulations of black hole-boson star binaries show that scalar self-interactions can suppress tidal disruption while radiative efficiency depends on the chosen potential.
citing papers explorer
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Massive boson stars: Stability and GW emission in head-on mergers
Quartically self-interacting massive boson stars are stable only up to the first mass maximum; their head-on mergers yield a boson-star remnant, a black hole at contact, or two black holes formed before contact, with radiated energy varying non-monotonically at strong coupling.
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Black Hole-Boson Star Binaries: Gravitational Wave Signals and Tidal Disruption
Numerical simulations of black hole-boson star binaries show that scalar self-interactions can suppress tidal disruption while radiative efficiency depends on the chosen potential.