Relativistic density functionals based on baryon-meson Lagrangians can be used to describe effectively dense matter in compact stars including hyperonic and Delta-resonance degrees of freedom. These can be supplemented with a first-order phase transition to quark matter at high densities to describe hybrid compact stars. I will discuss how the mass-radius and tidal deformability inferences constrain the current models of hyper nuclear and hybrid stars. I will go on to discuss the bulk viscosity of dense nucleonic matter in hot compact stars, which emerged in recent years as the leading dissipative channel in binary-neutron star merger simulations.
