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The vertical warp in the debris disk Beta Pictoris -- an inclined inner diskextending into a flat outer disk -- has long been interpreted as the signpostof a planet on an inclined orbit. Direct images spanning 2004-2010 haverevealed Beta Pictoris b, a planet with a mass and orbital distance consistentwith this picture. However, it was recently reported that the orbit of planet bis aligned with the flat outer disk, not the inclined inner disk, and thuslacks the inclination to warp the disk. We explore three scenarios forreconciling the apparent misalignment of the directly imaged planet BetaPictoris b with the warped inner disk of Beta Pictoris: observationaluncertainty, an additional planet, and damping of planet b's inclination. Wefind that, at the extremes of the uncertainties, the orbit of Beta Pictoris bhas the inclination necessary to produce the observed warp. We also find thatif planet b were aligned with the flat outer disk, it would prevent anotherplanet from creating a warp with the observed properties; therefore planet bitself must be responsible for the warp. Finally, planet b's inclination couldhave been damped by dynamical friction and still produce the observed diskmorphology, but the feasibility of damping depends on disk properties and thepresence of other planets. More precise observations of the orbit of planet band the position angle of the outer disk will allow us to distinguish betweenthe first and third scenario.

On the misalignment of the directly imaged planet {\beta} Pictoris b with the system's warped inner disk