Observational properties of Coherent Quantum Black Holes

TL;DR

This paper investigates the observational signatures of Coherent Quantum Black Holes, highlighting how their unique geometry affects geodesics, shadows, and accretion disk structures, which differ from classical black holes.

Contribution

It introduces a model of CQBH with a quantum core parameter and analyzes its geodesic properties and observational features, including shadows and lensing, using relativistic ray-tracing.

Findings

CQBH shadows have distinctive ring structures.

Geodesic behavior differs from Schwarzschild at short scales.

Simulations show observable differences in accretion disk images.

Abstract

We consider null and time-like geodesics around a spherically symmetric, non-rotating Coherent Quantum Black Hole (CQBH). The classical limit of the geometry of CQBH departs from that of the Schwarzschild spacetime at short scales and depends on one parameter $R_s$ which can be interpreted as the physical radius of the 'quantum' core. We study circular orbits, photon rings, and lensing effects and compare them with the Schwarzschild metric. Using the relativistic ray-tracing code GYOTO, we produce a simulation of the shadow and show that thin accretion disks around a CQBH possess unique ring structures that distinguish them from other theoretical models.