Protoneutron Star Convection Simulated with a New General Relativistic Boltzmann Neutrino Radiation Hydrodynamics Code

We investigate the protoneutron star (PNS) convection using our newly developed general relativistic Boltzmann neutrino radiation-hydrodynamics code. This is a pilot study for more comprehensive investigations later. As such, we take snapshot of PNS at 2.3 seconds after bounce from 1D cooling calculation and run simulation $\sim160\,\mathrm{ms}$ in 2D under axisymmetry. The original neglected entirely initial condition linearly unstable to convection. find that instigated there indeed expands inward being full-fledged. then settled quasi-steady state $\sim100\,\mathrm{ms}$, sustained by negative $Y_e$ gradient, which turn maintained emissions. It enhances luminosities mean energies all species neutrinos compared 1D. Taking advantage solver, analyze possible occurrence fast flavor conversion (FFC). found FFC likely occur regions, where lower, growth rate can be as high $\sim 10^{-1}\,{\mathrm{cm}^{-1}}$.