Numerical relativity in the decoupling limit reveals dynamical scalarization and spin-induced (de)scalarization during hyperbolic black hole encounters for both signs of the coupling.
Zoom-Whirl Orbits in Black Hole Binaries
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Zoom-whirl behavior has the reputation of being a rare phenomenon. The concern has been that gravitational radiation would drain angular momentum so rapidly that generic orbits would circularize before zoom-whirl behavior could play out, and only rare highly tuned orbits would retain their imprint. Using full numerical relativity, we catch zoom-whirl behavior despite dissipation. The larger the mass ratio, the longer the pair can spend in orbit before merging and therefore the more zooms and whirls seen. Larger spins also enhance zoom-whirliness. An important implication is that these eccentric orbits can merge during a whirl phase, before enough angular momentum has been lost to truly circularize the orbit. Waveforms will be modulated by the harmonics of zoom-whirls, showing quiet phases during zooms and louder glitches during whirls.
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Periodic orbits in Euler-Heisenberg black holes surrounded by perfect fluid dark matter produce burst-like gravitational wave signals whose amplitude and frequency content are modified by both dark matter density and QED parameters.
Gravitational waveforms from periodic orbits and QPOs around ENLMY black holes are derived and used with MCMC to constrain the Yukawa parameter and charge for microquasars and the galactic center.
The quantum parameter ξ in an asymptotically safe regular black hole shifts the innermost stable orbit, enhances whirl behavior in periodic geodesics, and produces amplitude-modulated millihertz gravitational-wave strains whose peak amplitude grows with ξ, placing them inside the sensitivity bands预计
Numerical study of timelike geodesics and millihertz gravitational waves from periodic orbits around a Schwarzschild black hole embedded in a (1,4,γ) Dehnen dark matter halo.
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