Speaker
Description
The investigation of the composition and evolution of rotating protoneutron stars (PNSs) encodes crucial information about their observable signatures while providing knowledge to advance observational investigations. We study the microphysical and macroscopic evolution of rotating PNSs using a relativistic mean-field model with density-dependent couplings that include finite temperature and evolving particle composition. The impact of rotation and neutrino-emission-driven changes in angular momentum, is analyzed through particle distributions, temperature profiles and sound speed, while global quantities such as gravitational mass, deformation, and energy distribution are simultaneously tracked.
We demonstrate that PNS deformation and thermal evolution are primarily controlled by angular momentum, mass, and composition. Rapid rotation and the appearance of exotic degrees of freedom, including hyperons and Δ resonances, enhance stellar deformation and lead to a reduction in core temperature. In contrast, slowly rotating massive neutron stars, such as PSR J0740+6620, remain nearly spherical.
These results place important constraints on the dense-matter equation of state and emphasize the need for a self-consistent treatment of rotation, mass-dependent compression, and composition in modeling protoneutron star evolution.
