  Galaxies are observed to be lopsided, meaning that they are more massive and
more extended along one direction than the opposite. In this work, we provide a
statistical analysis of the lopsided morphology of 1780 isolated satellite
galaxies generated by TNG50-1 simulation, incorporating the effect of tidal
fields from halo centres. The isolated satellites are galaxies without nearby
substructures whose mass is over $1\%$ of the satellites within their virial
radii. We study the radial alignment (RA) between the major axes of satellites
and the radial direction of their halo centres in radial ranges of $0$-$2R_{\rm
h}$, $2$-$5R_{\rm h}$ and $5$-$10R_{\rm h}$ with $R_{\rm h}$ being the stellar
half mass radius. According to our results, the RA is virtually undetectable in
inner and intermediate regions, yet it is significantly evident in outer
regions. We also calculate the far-to-near-side semi-axial ratios of the major
axes, denoted by $a_-/a_+$, which measures the semi-axial ratios of the major
axes in the hemispheres between backwards (far side) and facing (near side) the
halo centres. In all the radial bins of the satellites, the numbers of
satellites with longer semi-axes on the far side are found to be almost equal
to those with longer semi-axes on the near side. Therefore, the tidal fields
from halo centres play a minor role in the generation of lopsided satellites.
The long semi-major-axes radial alignment (LRA), i.e., an alignment between the
long semi-major-axes of satellite galaxies and the radial directions to their
halo centres, is further studied. No clear evidence of LRA is found in our
sample within the framework of $\Lambda$CDM Newtonian dynamics. Finally, we
briefly discuss the possible origins of the asymmetry of galaxies in TNG50-1.
