  We have investigated the rotational and the X-ray luminosity
($L_{\mathrm{x}}$) observations of 4U 1626--67 accumulated during the last four
decades. It has been recorded that the source underwent a torque reversal
twice. We have tried to understand whether this eccentrical sign-switch of the
period derivative ($\dot{P}$) of the source could be accounted for with the
existing torque models. We have found that the observed source properties are
better estimated with the distances close to the lower limit of the previously
predicted distance range ($5-13$ kpc). Furthermore, assuming an inclined
rotator, we have considered the partial accretion/ejection from the co-rotation
radius that leads different $L_{\mathrm{x}}$-$\dot{P}$ profiles than the
aligned rotator cases. We have concluded that the oblique rotator assumption
brings at least equally best fitting to the observed X-ray luminosity and the
rotational properties of 4U 1626--67. More importantly, the estimated change of
the mass accretion rate which causes the change in observed $L_{\mathrm{x}}$ of
4U 1626--67 is much less than that is found in an aligned rotator case. In
other words, without the need for a substantial modification of mass accretion
rate from the companion star, the range of the observed X-ray luminosity could
be explained naturally with an inclined magnetic axis and rotation axis of the
neutron star.
