In this work, we investigate how short-range correlations affect relativistic hadronic models at high densities, with direct consequences for the structure of neutron stars, both with and without dark matter content. Two versions of the model are examined; one with vector self-interactions up to second order (${\omega }_0^2$) and another including a fourth-order term (${\omega }_0^4$). We show that short-range correlations tend to soften the equation of state when only the quadratic term is present, but produce a noticeable stiffening once the ${\omega }_0^4$ term is included. The corresponding Tolman-Oppenheimer-Volkoff solutions for pure neutron stars indicate that short-range correlations reduce the maximum mass in the first case but increase it in the second. Extending the analysis to stars containing a fermionic dark matter component, within the two-fluid formalism, we verify that the same features appear in the respective mass-radius diagrams. In particular, the decrease of the maximum mass with increasing dark matter fraction is partly compensated by the short-range correlation effects in the hadronic sector for the model with the fourth-order term. In all cases, the resulting parametrizations are consistent with recent astrophysical constraints, including the joint NICER-XMM-Newton analyses of the pulsars PSR $\mathrm{J}0030+0451$ and PSR $\mathrm{J}0740+6620$, as well as the gravitational-wave event GW190425.

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• Dark matter
• General relativity
• Gravitational waves
• Nuclear matter in neutron stars