This work aims to understand what is the influence of the phase transition sharpness on the characteristics of neutron stars. Choosing the quark and the hadron phases models, we use a prescription that matches the two phases, in which we can control the sharpness of the transition through the value of a free parameter. In this work, we use the MIT bag model with repulsive vector interactions, and for the hadron phase, we use an equation of state consistent with the chiral effective field theory. We obtain hybrid equations of state with different sharpness of the phase transition and study how these changes affect the mass, radius, tidal deformability, and speed of sound in the star.
Organized by: Edoardo Giangrandi