  We investigate the morphology of the stellar halo (SH) in a sample of Milky
Way (MW) like galaxies in the TNG50 simulation. Using a local in shell
iterative method (LSIM) as the main approach, we explicitly show evidence of
twisting (in about 52% of halos) and stretching (in 48% of them) in the real
space. This is matched with the re-orientation observed in the eigenvectors of
the inertia tensor and gives us a clear picture of having a re-oriented SH. We
make a comparison between the shape profile of dark matter (DM) halo and SH and
quite remarkably see that their radial profiles are fairly close, especially at
small galactocentric radii where the stellar disk is located. This implies that
the DM halo is somewhat aligned with the stellar disk in response to the
baryonic potential. The level of alignment mostly decreases away from the
center. We study the impact of substructures in the orbital circularity
parameter. It is demonstrated that in some halos far away substructures are
counter-rotating compared with the central stars and may flip the sign of total
angular momentum and thus the orbital circularity parameter. Truncating them
above 150 kpc, however, retains the disky structure of the galaxy as per
initial selection. Including the impact of substructures in the shape of SH, we
explicitly show that their contribution is subdominant. Overlaying our
theoretical results to the observational constraints from previous literature,
we establish a fair agreement.
