Moments of inertia of neutron stars in relativistic mean field theory: the role of the isovector scalar channel

Understand

With the inclusion of the isovector scalar channel in the meson-nucleon couplings, taking DD-ME$\delta$ as an effective interaction, the moments of inertia of neutron stars possessing various stellar masses are studied within the density dependent relativistic mean field (RMF) theory.

• The isovector scalar channel contributes to the softening of the neutron-star matter equation of state (EOS) and therefore the reduction of the maximum mass and radius of neutron stars.
• Smaller values of the total moment of inertia $I$ and the crustal moment of inertia $\Delta{I}$ are then obtained in DD-ME$\delta$ via numerical procedure in comparison with those in other selected RMF functionals.
• In addition, the involvement of the isovector scalar channel lowers the thickness of the neutron star crust and its mass fraction as well.