We investigate the structural and physical properties of strange stars admixed with dark matter by modeling the total energy density as a weighted combination of quark matter and bosonic dark matter components regulated by a volume fraction. Both the components are assumed to be distributed throughout the star. The quark matter is described by a linear equation of state (EOS), whereas the bosonic dark matter follows an EOS with repulsive self-interactions. By combining these into a single effective EOS, we reduce the two-fluid system to an equivalent one-fluid model and numerically solve the Tolman-Oppenheimer-Volkoff (TOV) equations to obtain the mass-radius (M-R) relationship of the hybrid configuration. We systematically analyze how the stellar structure is modified by varying dark matter fractions, the mass of the dark matter particle and the self-repulsion coupling strength. Our results reveal distinct modifications to the M-R profiles and apparent phase behavior of the quark matter suggesting observable signatures that could offer insights into the properties of dark matter in extreme astrophysical environments. This model also provides a possible explanation for ultra-compact stars with small radii, such as XTE J1814-338, suggesting its potential nature as a hybrid star.
Chanda et al. (Tue,) studied this question.
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