Speaker
Description
Numerical simulations have been an important method for studying complex astrophysical scenarios, such as supernova explosions, showing that the remnant of core-collapse supernova rotates differentially at the initial phase of evolution. For neutron stars, differential rotation allows for significantly larger masses than rigid rotation. In our work, we study the stability of those objects and look for the most massive stable neutron stars that can be produced in core-collapse supernova. I will present the results of our studies. For a polytropic equation of state, we have estimated the limit of stability against radial oscillations for a selected sample of configurations. We considered a wide range of parameters and found stable configurations even twice as massive as the most massive non-rotating configuration.
