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