  We study the structure and basic physical properties of non-rotating dark
energy stars in Ho$\Check{\text{r}}$ava-Lifshitz (HL) gravity. The interior of
propsed stellar structure is made of isotropic matter obeys extended Chaplygin
gas EoS. The structure equations representing the state of hydrostatic
equilibrium i.e., generalize TOV equation in HL gravity is numerically solved
by using chosen realistic EoS. Next, we investigate the deviation of physical
features of dark energy stars in HL gravity as compared with general relativity
(GR). Such investigation is depicted by varying a parameter $\omega$, whereas
for $\omega\rightarrow \infty$ HL coincide with GR. As a results, we find that
necessary features of our stellar structure are significantly affected by
$\omega$ in HL gravity specifically on the estimation of the maximum mass and
corresponding predicted radius of the star. In conclusion, we can predict the
existence of heavior massive dark energy stars in the context of HL gravity as
compared with GR with not collapsing into a black hole. Moreover, we
investigate the stability of our proposed stellar system. By integrating the
modified perturbations equations in support of suitable boundary conditions at
the center and the surface of the stellar object, we evaluate the frequencies
and eigenfunctions corresponding to six lowest excited modes. Finally, we find
that physically viable and stable dark energy stars can be successfully
discussed in HL gravity by this study.
