  We present a three-species (H$^+$, O$^+$ and e$^-$) multi-fluid
magnetohydrodynamic (MHD) model, endowed with the requisite upper atmospheric
chemistry, that is capable of accurately quantifying the magnitude of oxygen
ion losses from "Earth-like" exoplanets in habitable zones, whose magnetic and
rotational axes are roughly coincidental with one another. We apply this model
to investigate the role of planetary obliquity in regulating atmospheric losses
from a magnetic perspective. For Earth-like exoplanets orbiting solar-type
stars, we demonstrate that the dependence of the total atmospheric ion loss
rate on the planetary (magnetic) obliquity is relatively weak; the escape rates
are found to vary between $2.19 \times 10^{26}$ s$^{-1}$ to $2.37 \times
10^{26}$ s$^{-1}$. In contrast, the obliquity can influence the atmospheric
escape rate ($\sim$ $10^{28}$ s$^{-1}$) by more than a factor of $2$ (or
$200\%$) in the case of Earth-like exoplanets orbiting late-type M-dwarfs.
Thus, our simulations indicate that planetary obliquity may play a
weak-to-moderate role insofar as the retention of an atmosphere (necessary for
surface habitability) is concerned.
