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General Approach on Shadow Radius and Photon Spheres in Asymptotically Flat Spacetimes and the Impact of Mass-Dependent Variations
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Recent observations of black hole shadows have revolutionized our ability to probe gravity in extreme environments. This manuscript presents a novel analytic method to calculate, in leading-order terms, the key parameters of photon sphere and shadow radius. This method offers advantages for complex metrics where traditional approaches are cumbersome. We further explore the impact of black hole mass on the photon sphere radius, providing insights into black hole interactions with their surroundings. Our findings contribute significantly to black hole physics and gravity under extreme conditions. By leveraging future advancements in observations, such as the next-generation Event Horizon Telescope (ngEHT), this work paves the way for even more precise tests of gravity near black holes.
Forward citations
Cited by 3 Pith papers
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Shadow of the generalized Vaidya black hole
For self-similar Husain black holes, the barotropic index α controls the shadow: α<1/2 enlarges it, α>1/2 shrinks it, with a quasistatic influx criterion for the time-dependent case.
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Signatures of cubic gravity in the strong regime
Einsteinian cubic gravity shrinks (grows) black hole horizons for positive (negative) coupling and shifts the photon sphere enough that SgrA* shadow observations can bound the coupling to approximately 0.1.
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Regular Black Hole Formation and Gamma-Ray Burst from Matter Conversion
The formation of a regular black hole could release gamma-ray-burst-scale energy only if its singularity-avoiding core is a weak perturbation of Schwarzschild.
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