  We focus attention on the Oe/Be stars to test the concept that the disks of
these stars form by magnetic channeling of wind material toward the equator.
Calculations are made of the X-rays expected from the Magnetically Torqued Disk
(MTD) model for Be stars discussed by Cassinelli et al. (2002), by Maheswaran
(2003), and by Brown et al. (2004). The dominant parameters in the model are
the $\beta$ value of the velocity law, the rotation rate of the star, $S_o$,
and the ratio of the magnetic field energy density to the disk gravitational
energy density, $\gamma$.
  The model predictions are compared with the $ROSAT$ observations obtained for
an O9.5 star $\zeta$ Oph from \Berghofer et al. (1996) and for 7 Be stars from
Cohen et al. (1997). Extra considerations are also given here to the well
studied Oe star $\zeta$ Oph for which we have $Chandra$ observations of the
X-ray line profiles of the triad of He-like lines from the ion Mg XI.
