A new cosmological zoom-in simulation of a major merger between two 10^9 solar-mass halos at z~11 finds that sustained super-Eddington accretion occurs only when black-hole feedback is artificially disabled. With realistic radiative plus kinetic feedback included, gas inflows triggered by the merger are rapidly expelled, limiting black-hole growth to negligible levels after the initial seeding episode. The study employs high-resolution zoom simulations with three accretion regimes (ADAF, thin-disk, and super-Eddington) and multiple feedback channels; kinetic winds dominate regulation. This single-merger case challenges the widespread assumption, adopted in many semi-analytic models and large-volume simulations, that galaxy mergers are the dominant trigger for the extreme accretion needed to explain JWST-detected 10^6–10^7 solar-mass black holes at z>8. Earlier work on more massive systems at lower redshift (e.g., Di Matteo et al. 2005 in Nature) showed mergers can drive inflows, yet those runs lacked the kinetic jet component now shown to be decisive at high redshift. A separate analysis of the IllustrisTNG50 volume (Weinberger et al. 2018) similarly found that kinetic feedback quenches black-hole growth below halo masses of ~10^12 solar masses, supporting the present result that low-mass mergers at cosmic dawn are inefficient. The preprint therefore highlights a key limitation: current seeding prescriptions and feedback implementations may still be too simplistic to capture brief, merger-induced super-Eddington windows that could exist in rarer, higher-mass environments.