  The 80 high-mass X-ray binary (HMXB) pulsars that are known to reside in the
Magellanic Clouds (MCs) have been observed by the XMM-Newton and Chandra X-ray
telescopes on a regular basis for 15 years, and the XMM-Newton and Chandra
archives contain nearly complete information about the duty cycles of the
sources with spin periods P_S < 100 s. We have rerprocessed the archival data
from both observatories and we combined the output products with all the
published observations of 31 MC pulsars with P_S < 100 s in an attempt to
investigate the faintest X-ray emission states of these objects that occur when
accretion to the polar caps proceeds at the smallest possible rates. These
states determine the so-called propeller lines of the accreting pulsars and
yield information about the magnitudes of their surface magnetic fields. We
have found that the faintest states of the pulsars segregate into five discrete
groups which obey to a high degree of accuracy the theoretical relation between
spin period and X-ray luminosity. So the entire population of these pulsars can
be described by just five propeller lines and the five corresponding magnetic
moments (0.29, 0.53, 1.2, 2.9, and 7.3, in units of 10^30 G cm^3).
