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We have compiled a comprehensive library of all X-ray observations ofMagellanic pulsars carried out by {\it XMM-Newton}, {\it Chandra}, and {\itRXTE} in the period 1997-2014. In this work, we use the data from 53 high-massBe/X-ray binaries in the Small Magellanic Cloud to demonstrate that thedistribution of spin-period derivatives vs. spin periods of spinning-downpulsars is not at all different than that of the accreting spinning-up pulsars.The inescapable conclusion is that the up and down samples were drawn from thesame continuous parent population, therefore Be/X-ray pulsars that are spinningdown over periods spanning 18 years are in fact accreting from retrogradedisks. The presence of prograde and retrograde disks in roughly equal numberssupports a new evolutionary scenario for Be/X-ray pulsars in their spinperiod-period derivative diagram.

Retrograde Accretion Disks in High-Mass Be/X-ray Binaries