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In this work, we study the effects of nuclear symmetry energy slope onneutron star dense matter equation of state and its impact on neutron starobservables (mass-radius, tidal response). We construct the equation of statewithin the framework of covariant density functional theory implementingcoupling schemes of non-linear and density-dependent models with viability ofheavier non-nucleonic degrees of freedom. The slope of symmetry energyparameter ($L_{\text{sym}}$) is adjusted following density-dependence ofisovector meson coupling to baryons. We find that smaller values of$L_{\text{sym}}$ at saturation favour early appearance of $\Delta$-resonancesin comparison to hyperons leading to latter's threshold at higher matterdensities. We also investigate the dependence of $L_{\text{sym}}$ on tidaldeformability and compactness parameter of a $1.4~M_\odot$ neutron star fordifferent equation of states and observe similar converging behaviour forlarger $L_{\text{sym}}$ values.

Influence of the nuclear symmetry energy slope on observables of compact stars with $\Delta$-admixed hypernuclear matter