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What does a binary black hole merger look like?
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We present a method of calculating the strong-field gravitational lensing caused by many analytic and numerical spacetimes. We use this procedure to calculate the distortion caused by isolated black holes and by numerically evolved black hole binaries. We produce both demonstrative images illustrating details of the spatial distortion and realistic images of collections of stars taking both lensing amplification and redshift into account. On large scales the lensing from inspiraling binaries resembles that of single black holes, but on small scales the resulting images show complex and in some cases self-similar structure across different angular scales.
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Cited by 4 Pith papers
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Polarization-dependent observational signatures of Weyl-coupled photons around a black hole
Weyl-coupled photons on Schwarzschild produce a polarization-split double shadow (62% edge separation at α/M²=0.75) and a parity-protected backward birefringence signal that vanishes at α=0.
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Analytic thin disks and rings in a class of nonasymptotically flat static spacetimes
External quadrupolar distortion imprints on orbital dynamics and accretion structure in thin disks around deformed compact objects, with the radiating region's outer edge tied to the radiation-to-gas pressure transition.
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Effect of a second compact object on stable circular orbits
In the Majumdar-Papapetrou two-black-hole spacetime, the mass ratio of the two holes divides into four regimes separated by three critical values that control the existence and topology of stable circular orbits.
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Effect of gravitational wave on shadow of a Schwarzschild black hole
Numerical ray tracing shows that a first-order gravitational perturbation makes a Schwarzschild black hole shadow oscillate, stretch, and develop self-similar fractal boundary structures over time.
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