On the Neutrino Distributions in Phase Space for the Rotating Core-Collapse Supernova Simulated with a Boltzmann-Neutrino-Radiation-Hydrodynamics Code

摘要: With the Boltzmann-radiation-hydrodynamics code, which we have developed to solve numerically Boltzmann equations for neutrino transfer, Newtonian hydrodynamics equations, and self-gravity simultaneously consistently, simulate collapse of a rotating core progenitor with zero-age-main-sequence mass $11.2\,M_\odot$ shelluler rotation $1\,{\rm rad\,s^{-1}}$ at center. We pay particular attention in this paper distribution phase space, is affected by rotation. By solving directly, can assess rotation-induced distortion angular momentum gives rise rotational component flux. compare Eddington tensors calculated both from raw data M1-closure approximation. demonstrate that tensor determined complicated interplays fluid velocity interactions M1-closure, assumes factor flux factor, fails fully capture aspect, especially vicinity shock. find error reaches $\sim 20\%$ our simulation. This due not resolution but different dependence factors on profile function, hence modification closure relation needed.