Recent cross-matching of faint far-infrared sources between the 1983 IRAS and 2006 AKARI all-sky surveys has produced a candidate pair separated by approximately 42–69.6 arcmin, interpreted as possible orbital motion of a massive ninth planet at 500–700 AU. We demonstrate that this interpretation is unnecessary and dynamically inconsistent. Within the Webb Mechanical Model, the outer solar system remains angularly locked to the central anchor (Sol) via hierarchical coupling. At these distances, objects must maintain higher orbital speeds to stay in phase, but lack sufficient coalesced mass for planetary-scale drag. The observed “clicks” are instead rare thermal flashes from irregular, tumbling icy debris—remnants of SMDS foundry extrusion and DoPE events—in a sparse, mostly invisible population. Different chunks flash into detection threshold when a reflective/hot facet aligns with the Sun and observer; rotation hides them for decades. The apparent shift is selection bias, not a single orbit. Moreover, any perturber massive enough to sculpt the observed Kuiper Belt clustering would induce detectable secular perturbations on inner planets and a measurable solar barycenter wobble—effects absent in high-precision data. A body scaled to Jupiter ×5 (∼1,590 M⊕) at ≤900 AU would produce catastrophic wobble incompatible with observations. The Sedna gap and assumed Oort Cloud create an additional paradox: mainstream models require Planet 9 to “capture” distant baryonic debris yet assume an Oort Cloud exists naturally at even greater distances. Even Sol—the system’s largest body—fails to capture small interstellar objects (e.g., 1I/‘Oumuamua on a hyperbolic trajectory), proving capture is unnecessary. The debris-field model explains all data without undetectable mass.
Matt Webb (2026) studied this question.