We investigate the impact of slope of the symmetry energy ($L$) on asymmetric nuclear dense matter (neutron star) characteristics, specifically focusing on the maximum mass, radius, and dimensionless tidal deformability of a canonical mass star. To this aim, we consider a set of relativistic mean field (RMF) models based on the BSRV-CPREX parametrization [Phys. Rev. C 107, 055801 (2023)] wherein the interaction between nucleons and the rho meson, quantified by $g_{\rho N}$, as well as the vector meson mixing interaction (${\omega }^2\text{−}{\rho }^2$), represented by ${\mathrm{\Lambda }}_{\omega \rho }$, are concurrently adjusted to achieve a wide range of $L$ at saturation density ${\rho }_0$ while keeping the isoscalar nuclear matter properties fixed at ${\rho }_0$. We formulate a set of equations of state (EoSs) for $\beta$-equilibrated nucleonic matter corresponding to these RMF models, employing these EoSs to examine the influence of $L$ on neutron star attributes, including maximum mass, radius, and dimensionless tidal deformability associated with canonical mass neutron stars ($1.4M_{\odot }$). The analysis of our results suggests that various neutron star characteristics have a pronounced dependence on the slope of symmetry energy. The effect of $L$ on the threshold density and mass for the onset of the direct Urca process is also examined.

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• Asymmetric nuclear matter
• Nuclear astrophysics
• Nuclear matter in neutron stars
• Symmetry energy