  We have compiled a comprehensive library of all X-ray observations of
Magellanic pulsars carried out by {\it XMM-Newton}, {\it Chandra}, and {\it
RXTE} in the period 1997-2014. In this work, we use the data from 53 high-mass
Be/X-ray binaries in the Small Magellanic Cloud to demonstrate that the
distribution of spin-period derivatives vs. spin periods of spinning-down
pulsars 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 the
same continuous parent population, therefore Be/X-ray pulsars that are spinning
down over periods spanning 18 years are in fact accreting from retrograde
disks. The presence of prograde and retrograde disks in roughly equal numbers
supports a new evolutionary scenario for Be/X-ray pulsars in their spin
period-period derivative diagram.
