Standard models of stellar angular momentum evolution fail to describe the rotation of stars older than the Sun, which exhibit anomalously rapid rotation in Kepler and TESS field samples. This phenomenon, known as weakened magnetic braking (WMB), is hypothesized to stem from a fundamental shift in magnetic morphology. In this talk, I will present a uniform reanalysis of a broad sample of stars (late F to early K) using direct spectropolarimetric magnetic field measurements and X-ray inferred mass-loss rates to bypass traditional, indirect activity proxies. The results demonstrate an abrupt, two order of magnitude decrease in wind braking torque as the Rossby number approaches a critical point slightly above the solar value (Ro ~ 1.01 Ro_sun). Notably, the results indicate that the Sun is already well within this transition, with its current wind braking torque significantly suppressed relative to the predictions of traditional spin-down models. The transition is clearly reflected in both large-scale magnetic field strengths and X-ray luminosities, signaling a disruption of global organizing flows and weakened coronal heating. These findings have been interpreted as evidence of a rotational threshold for the influence of Coriolis forces on global convective patterns, a transition that can be modeled as a supercritical Hopf bifurcation where global dynamo excitation ceases. This work provides a physical basis for the observed "flat-activity" state in old stars and establishes a new paradigm for the limitations of gyrochronology beyond the middle of main-sequence lifetimes.