Speaker
Description
In this work, we investigate the combined effects of pressure anisotropy and the inclusion of $\Delta$ resonances on the structural properties of compact stars. The study is performed within a relativistic hadronic framework that incorporates $\Delta$ baryons, where the equation of state (EoS) is constructed under the conditions of charge neutrality and $\beta$-equilibrium.
Pressure anisotropy, which may arise due to extreme densities, strong interactions, or possible phase transitions in dense matter, is introduced through phenomenological anisotropic models that allow for a distinction between radial and tangential pressures. The modified Tolman--Oppenheimer--Volkoff equations are solved self-consistently to obtain the mass--radius relations of anisotropic compact stars in the presence of $\Delta$ resonances. We systematically analyze the sensitivity of stellar properties, such as maximum mass and radius, to the anisotropy parameter and the onset of $\Delta$ particles.
