Abstract We systematically investigate the observable properties and stellar configurations of dark matter (DM)-admixed quark stars (DQSs) by combining the confined-isospin-density-dependent-mass (CIDDM) model with the generic bosonic self-interacting DM model. Currently, the DM particles mass remains undetermined, we find that heavier DM particles lead to a softer equation of state (EOS) for pure dark star, a higher adiabatic index and a lower speed of sound, resulting in a reduced maximum gravitational mass. Meanwhile, our results show that both the DM particles mass and DM fraction significantly affect the properties of quark stars including the mass, radius, tidal deformability and the types of stellar configurations. For lighter DM particles, DQSs tend to form DM-halo configurations, whereas for heavier particles, DM-core configurations become dominant. Moreover, within the CIDDM framework, we explore whether two recently observed peculiar objects, HESS J1731-347 and the secondary component of PSR J0514-4002E, could be DQSs, and identify the allowed DM parameter space compatible with their observational data and the corresponding stellar configurations. Our findings suggest that DQSs remain viable candidates for explaining certain compact astrophysical objects and may offer valuable insights into the DM nature.
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