  Planets and moons reorient in space due to mass redistribution associated
with various types of internal and external processes. While the equilibrium
orientation of a tidally locked body is well understood, much less explored are
the dynamics of the reorientation process (or true polar wander, TPW, used here
for the motion of either the rotation or the tidal pole). This is despite their
importance for predicting the patterns of TPW-induced surface fractures, and
for assessing whether enough time has passed for the equilibrium orientation to
be reached. The only existing, and relatively complex numerical method for an
accurate evaluation of the reorientation dynamics of a tidally locked body was
described in a series of papers by Hu et al. (2017a,b, 2019). Here we
demonstrate that an identical solution can be obtained with a simple approach,
denoted as ow||mMIA, because, contrary to previous claims, during TPW the tidal
and the rotation axes closely follow respectively the minor and the major axes
of the total, time-evolving inertia tensor. Motivated by the presumed
reorientation of Pluto, the use of the ow||mMIA method is illustrated on
several test examples. In particular, we analyze whether reorientation paths
are curved or straight when the load sign and the mass of the host body are
varied. When tidal forcing is relatively small, the paths of negative anomalies
(e.g.~basins) towards the rotation pole are highly curved, while positive loads
may reach the sub- or anti-host point in a straightforward manner. Our results
suggest that the Sputnik Planitia basin cannot be a negative anomaly at present
day, and that the remnant figure of Pluto must have formed prior to the
reorientation. Finally, the presented method is complemented with an energy
balance that can be used to test the numerical solution.
