Time-domain evolutions demonstrate that the nonlinear scalar ergoregion instability saturates via a weakly turbulent direct cascade transferring energy to small scales and populating higher-order azimuthal modes on the stable light ring.
Rotating Boson Stars and Q-Balls
3 Pith papers cite this work. Polarity classification is still indexing.
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abstract
We consider axially symmetric, rotating boson stars. Their flat space limits represent spinning Q-balls. We discuss their properties and determine their domain of existence. Q-balls and boson stars are stationary solutions and exist only in a limited frequency range. The coupling to gravity gives rise to a spiral-like frequency dependence of the boson stars. We address the flat space limit and the limit of strong gravitational coupling. For comparison we also determine the properties of spherically symmetric Q-balls and boson stars.
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Hartree quantum fluctuations in 3+1D simulations of the Friedberg-Lee-Sirlin model produce a regime where fluctuations carry significant Noether charge, periodic charge exchange occurs, and some classically stable Q-balls become unstable.
Bayesian analysis shows current near-IR astrometry data cannot distinguish massive boson stars from Schwarzschild black holes for Sgr A*.
citing papers explorer
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Weakly turbulent saturation of the nonlinear scalar ergoregion instability
Time-domain evolutions demonstrate that the nonlinear scalar ergoregion instability saturates via a weakly turbulent direct cascade transferring energy to small scales and populating higher-order azimuthal modes on the stable light ring.
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Quantum-Corrected Q-balls in the Friedberg-Lee-Sirlin Model
Hartree quantum fluctuations in 3+1D simulations of the Friedberg-Lee-Sirlin model produce a regime where fluctuations carry significant Noether charge, periodic charge exchange occurs, and some classically stable Q-balls become unstable.
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Bayesian Analysis of Massive Boson Star Models for Sagittarius A* Using Near-Infrared Astrometry Data
Bayesian analysis shows current near-IR astrometry data cannot distinguish massive boson stars from Schwarzschild black holes for Sgr A*.