Stability of spinning bosonic stars

Enlace meet

Abstract: This talk will discuss recent results regarding the stability of spinning bosonic stars. Using numerical-relativity simulations we will show that scalar and vector bosonic stars have different stability properties. For all unstable models the energy density displays a toroidal morphology. These transient models develop a dynamical bar-mode instability which closely resembles what happens for rotating neutron stars. The instability triggers the emission of gravitational waves which might be within reach of future experiments. Recent proposals to quench the instability will also be discussed.