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We present the results of N-body simulations meant to reproduce the long-termeffects of mutually inclined exoplanets on debris disks, using the HD 202628system as a proxy. HD 202628 is a Gyr-old solar-type star that possesses adirectly observable, narrow debris ring with a clearly defined inner edge andnon-zero eccentricity, hinting at the existence of a sculpting exoplanet. Theeccentric nature of the disk leads us to examine the effect on it over Gyrtimescales from an eccentric and inclined planet, placed on its orbit throughscattering processes. We find that, in systems with dynamical timescales akinto that of HD 202628, a planetary companion is capable of completely tiltingthe debris disk. This tilt is preserved over the Gyr age of the system.Simulated observations of our models show that an exoplanet around HD 202628with an inclination misalignment $\gtrsim\,10$ degrees would cause the disk tobe observably diffuse and broad, which is inconsistent with ALMA observations.With these observations, we conclude that if there is an exoplanet shaping thisdisk, it likely had a mutual inclination of less than 5 degrees with theprimordial disk. Conclusions of this work can be either applied to debris disksappearing as narrow rings (e.g., Fomalhaut, HR 4796), or to disks that arevertically thick at ALMA wavelengths (e.g., HD 110058).

Long-term Evolution of Warps in Debris Disks -- Application to the Gyr-old system HD 202628