2018/06/30 by Kuo-Chuan 國全 Pan 潘, Kuo-Chuan Pan, Carlos Mattes +6 · 1 citation
Physics and Astronomy · #Convection #Convection–diffusion equation #Gamma-ray bursts and supernovae #Isotropy #Neutrino #Neutrino Physics Research #Neutrino oscillation #Particle physics theoretical and experimental studies #Shock (circulatory) #Supernova #Type II supernova #astro-ph.HE
paper · pdf · doi:10.1088/1361-6471/aaed51
28 pages, 11 figures, accepted by J. Phys. G focus issue on core-collapse supernovae
openalex created_date 2018/07/10 · arxiv created 2018/10/15 · openalex publication_date 2018/11/01 · arxiv updated 2018/12/05 · openalex updated_date 2026/08/05
Abstract Neutrinos play a crucial role in the core-collapse supernova (CCSN) explosion mechanism. The requirement of accurately calculating the transport of neutrinos makes simulations of the CCSN mechanism extremely challenging and computationally expensive. Historically, this stiff challenge has been met by making approximations to the full transport equation. In this work, we compare CCSN simulations in one- and two-dimensions with three approximate neutrino transport schemes, each implemented in the FLASH simulation framework. We compare a two-moment M1 scheme with an analytic closure (M1), the isotropic diffusion source approximation (IDSA), and the advanced spectral leakage method. We identify and discuss the advantages and disadvantages of each scheme. For each approximate transport scheme, we use identical grid setups, hydrodynamics, and gravity solvers to investigate the transport effects on supernova shock dynamics and neutrino quantities. We find that the transport scheme has a small effect on the evolution of protoneutron star (PNS) radius, PNS mass, and the mass accretion rate. The neutrino luminosities, mean energies, and shock radii have a ∼10%–20% quantitative difference but the overall qualitative trends are fairly consistent between all three approximations. We find larger differences in the gain region properties, including the gain region mass and the net heating rate in the gain region, as well as the strength of PNS convection in the core. We investigate the progenitor, nuclear equation of state, and stochastic perturbation dependence of our simulations and find similar magnitudes of impact on key quantities. We also compare the computational expense of the various approximations.