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The current observational properties of neutron stars have not definitivelyruled out the possibility of dark matter. In this study, we primarily focus onexploring correlations between the dark matter model parameters and differentneutron star properties using a rich set of EOSs. We adopt a two-fluid approachto calculate the properties of neutron stars. For the nuclear matter EOS, weemploy several realistic EOS derived from the relativistic mean field model(RMF), each exhibiting varying stiffness and composition. In parallel, we lookinto the dark matter EOS, considering fermionic matter with repulsiveinteraction described by a relativistic mean field Lagrangian. A reasonablerange of parameters is sampled meticulously. Interestingly, our results reveala promising correlation between the dark matter model parameters and stellarproperties, particularly when we ignore the uncertainties in the nuclear matterEOS. However, when introducing uncertainties in the nuclear sector, thecorrelation weakens, suggesting that the task of conclusively constraining anyparticular dark matter model might be challenging using global propertiesalone, such as mass, radius, and tidal deformability. Notably, we find thatdark-matter admixed stars tend to have higher central baryonic density,potentially allowing for non-nucleonic degrees of freedom or direct Urcaprocesses in stars with lower masses. There is also a tantalizing hintregarding the detection of stars with the same mass but different surfacetemperatures, which may indicate the presence of dark matter. With our robustand extensive dataset, we delve deeper and demonstrate that even in thepresence of dark matter, the semi-universal C-Love relation remains intact.

Exploring robust correlations between fermionic dark matter model parameters and neutron star properties: A two-fluid perspective