  Kilonovae are generally believed to originate from the ejecta of binary
neutron stars (NSs) or black hole and NS mergers. Free neutrons might be
retained in the outermost layer of the ejecta to produce a precursor via
$\beta$-decay. During the propagation of kilonovae to observers, a small
percentage of them might be gravitationally lensed by foreground objects. In
this paper, three lens models, i.e., the point-mass model, the singular
isothermal sphere (SIS) model, and the Chang-Refsdal model, were taken into
consideration to explore the light curves and polarizations of gravitationally
lensed kilonovae. We found that if the time delay between two images exceeds
the ejecta heating timescale for the lens mass $\sim 10^{10}~M_\odot$ in the
SIS model, a tiny bump-like signal will be generated in the light curve, and
the total luminosity will be magnified in all cases. The polarization of lensed
kilonovae is significantly enhanced in most cases. Future detections of lensed
kilonovae will impose constraints on the morphology of the ejecta and aid in
the determination of the nature of compact object mergers and the search for
strong gravitational lenses.
