Radial pulsations, moment of inertia and tidal deformability of dark energy stars

We construct dark energy stars with Chaplygin-type equation of state (EoS) in the presence anisotropic pressure within framework Einstein gravity. From classification established by Iyer et al. [Class. Quantum Grav. 2, 219 (1985)], we discuss possible existence isotropic as compact objects. However, there is possibility constructing ultra-compact for sufficiently large anisotropies. investigate stellar stability against radial oscillations, and also determine moment inertia tidal deformability these stars. find that usual static criterion $dM/d\rho_c >0$ still holds since squared frequency fundamental pulsation mode vanishes at critical central density corresponding to maximum-mass configuration. The dependence Love number on anisotropy parameter $\alpha$ examined. show surface gravitational redshift, dimensionless undergo significant changes due pressure, primarily high-mass region. Furthermore, light detection waves GW190814, explore describing secondary component such event a stable star anisotropy.