Models of planet formation and evolution predict that giant planets form efficiently in protoplanetary disks, that most of these migrate rapidly to the disks inner edge, and that, if the arriving planets mass is $lesssim$ Jupiters mass, it could remain stranded near that radius. We argue that such planets would be ingested by tidal interaction with the host star on a timescale $lesssim1,$Gyr, and that, in the case of a solar-type host, this would cause the stellar spin to approach the direction of the ingested planets orbital axis even if the two were initially highly misaligned. Primordially misaligned stars whose effective temperatures are $gtrsim6250,$K cannot be realigned in this way because, in contrast with solar-type hosts, their angular momenta are typically higher than the orbital angular momentum of the ingested planet as a result of inefficient magnetic braking and of a comparatively large moment of inertia. Hot Jupiters located farther out from the star can contribute to this process, but their effect is weaker because the tidal interaction strength decreases rapidly with increasing semimajor axis. We demonstrate that, if $sim50%$ of planetary systems harbored a stranded hot Jupiter, this scenario can in principle account for (1) the good alignment exhibited by planets around cool stars irrespective of the planets mass or orbital period, (2) the prevalence of misaligned planets around hot stars, (3) the apparent upper bound on the mass of hot Jupiters on retrograde orbits, and (4) the inverse correlation between stellar spin periods and hot-Jupiter masses.
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