A preprint posted to arXiv in May 2026 (Vincentelli et al.) reports the first quantitative linear correlation between Type-C QPO fractional rms amplitude and radio-derived jet inclination in black-hole LMXBs, extending up to 8 Hz. The analysis combines RXTE archival light curves with HXMT timing data and updated inclination constraints from radio imaging, revealing systematically lower amplitudes on outburst decay than rise at fixed frequency. This strengthens geometric models in which a precessing inner hot flow modulates the observed flux, but only if spin-orbit misalignment reaches at least 10-15 degrees. The study does not specify exact sample size, yet draws on a modest set of well-observed systems; as an unreviewed preprint it lacks independent verification of the inclination measurements and may be affected by selection biases toward brighter, better-monitored outbursts. Connecting this result to earlier work (Motta et al. 2015 on inclination-dependent rms and Ingram et al. 2016 on Lense-Thirring precession) shows that QPO strength now supplies an observable proxy for the same misalignment thought to collimate jets, directly linking two previously separate accretion-ejection threads. Future multi-messenger campaigns pairing X-ray timing with VLBI jet imaging or gravitational-wave ringdown measurements could test whether the same misalignment governs both QPO amplitude and jet power across the mass scale.