Black Hole Shadows Put Quantum Gravity to the Test ⚡ экспресс
Using the Event Horizon Telescope, shadows of supermassive black holes M87* and Sgr A* were investigated to test loop quantum gravity effects. Rotating black holes with holonomy corrections (RHCBH) were analyzed. It was found that the quantum parameter b increases the shadow size: prograde photon orbits move outward, indicating weakened effective gravity near the center. Unlike Kerr naked singularities, RHCBH produce closed shadow rings even without an event horizon—thanks to unstable circular photon orbits. The Kumar–Ghosh method, relying on shadow area A and its oblateness D, allowed constraining b from observations. For M87* (inclination 17°): b ≤ 0.1319 M at a=0 and b ≤ 0.421 M at a=0.784 M. For Sgr A* (inclination 50°): b ≤ 0.5764 M at a=0 and b ≤ 0.7482 M at a=0.6253 M. Nonzero values of b are not ruled out by data, making RHCBH competitive candidates for astrophysical black holes.
The shadow of a black hole is not just a silhouette. It's the edge of the abyss, where space and time are twisted so tightly that even light is forced to swirl like a wood chip in a whirlpool. This 'cosmic whirlpool' arises from the monstrous mass warping spacetime.
Physicists tested what would happen if quantum effects—tiny corrections from loop quantum gravity theory, where space itself is made of microscopic loops—are added to this whirlpool. Calculations showed that quantum corrections barely perceptibly widen the shadow. But more importantly, even if you remove the 'drain hole,' i.e., the event horizon, the funnel remains closed, and the shadow stays a ring. The real surprise: inside such a black hole, there's no singularity point, just an entangled tangle of loops.
🎯 Light in a black hole's shadow can loop around, creating an infinite series of reflections, like in a hall of mirrors.
🎬 In 'Interstellar,' Gargantua's shadow was modeled using classical equations; quantum corrections would make it slightly more oval.