Black Holes as Super-Stars: A Relativistic and Numerical Assessment of the Quantum Gravity Theory (QGT) Model

The Super-Star proposal interprets an ultracompact object as a self-gravitating configuration of a complex scalar field whose attractive quartic and repulsive sextic interactions may support a regular high-density core. This paper develops a covariant Einstein-scalar formulation, derives the static spherical structure equations and their anisotropic Tolman-Oppenheimer-Volkoff form, and sets out the conditions required for a horizonless compact object, a photon sphere, a shadow, dynamical stability, and gravitational-wave signatures. The distinction between an event horizon, a material surface, a photon circular orbit, a critical impact parameter, and the proposed QGT "Zero Orbit" is made explicit. A rotating perturbative extension is also assessed using computed l = 1 scalar modes, an axial frame-dragging response, a spherical l = 0 backreaction, and an even-parity l = 2 sector. The numerical evidence is reported with residuals and convergence data rather than being promoted to a complete nonlinear rotating solution. In the reference dimensionless model, the scanned spherical backgrounds remain below the photon-orbit condition; hence the present computations do not establish a black-hole-like shadow or an event-horizon replacement. The analysis identifies which parts reproduce standard Einstein-Klein-Gordon theory, which QGT claims remain hypotheses, and which additional equations and tests are needed for an independently predictive theory. The result is a reproducible research framework, not a claim that singularity avoidance, information recovery, polar jets, or observational equivalence have already been proved.