Velocity-resolved Relationship between Filamentary H I Structure and Magnetic-field Orientation in the Orion-Eridanus Superbubble Region

Magnetic fields are a fundamental property of diffuse interstellar medium． Previous studies have shown that filamentary H I structure often follows the plane-of-sky magnetic field inferred from polarized dust emission． Leveraging high-sensitivity FAST/CRAFTS H I survey and Planck 353 GHz dust polarization, we target the Orion--Eridanus super-bubble environment and map relative orientation between H I filaments and dust-inferred magnetic field across v_LSR= −15 to +15 km/s⁻¹． We find a clear environmental bifurcation: exterior to the projected shell, low-velocity gas (−15 ≤ v_LSR < 0 km/s⁻¹) shows large and spatially coherent misalignment (|∆θ|med ≈ 45°), whereas higher-velocity exterior gas aligns significantly better (|∆θ|med ≈ 28°)． The interior remains comparably well-aligned across all velocities, with little velocity dependence． Therefore broad H I-dust alignment commonly seen in velocity-integrated studies does not apply uniformly to all kinematic components in the Orion-Eridanus environment． The spatially coherent low-velocity exterior structure represents a distinct component with enhanced misalignment, providing a new observational clue to the origin of geometrically differentiated atomic gas in a feedback-shaped environment.