  We employ the recently improved description of dense baryonic matter within
the Witten-Sakai-Sugimoto model to construct neutron stars. In contrast to
previous holographic approaches, the presence of an isospin asymmetry allows us
to implement beta equilibrium and electric charge neutrality. As a consequence,
we are able to model the crust of the star within the same formalism and
compute the location of the crust-core transition dynamically. After showing
that a simple pointlike approximation for the baryons fails to satisfy
astrophysical constraints, we demonstrate that our improved description does
account for neutron stars that meet the current experimental constraints for
mass, radius, and tidal deformability. However, we also point out tensions in
the parameter fit and large-$N_c$ artifacts and discuss how to potentially
resolve them in the future.
