Comparison Between Two Kinds Of Type Ⅱ Supernova Explosion

A brief review of general theory of the iron-core collapse supernova by one dimensional spherically symmetric model is presented in this paper, including the evolution of stars and progenitor stars, the iron-core collapses, shock-wave formation and propagation as well as the neutrino effect. Then,in this paper the influence of different equations of state on the supernovae of iron-core collapse are discussed and the equation of state of two different symmetry equations are introduced. In addition, we also compares the differences from two numerical results of iron-core collapse supernova, where one is Wgxnu model and the other is SNEC model that from Tobias Fischer et al. Wgxnu model is based on SNⅡ-WLYW89 which is developed by Chinese researcher group of Yiren Wang in the equation of state (Wang.EOS) of Wgxnu model, we removed "the equivalent thickness method",adjusted the neutrino leakage equation and added the equation of symmetrical energy. To adjust the neutrino leaked equation we use b=5, bf=0.05 as the best parameters. The symmetric energy of homogeneous nuclear matter in numerical simulation of supernova is replaced by the density-dependence form of symmetry energy to asymmetric nuclear matter from research team Baoan Li. supernova numerical simulation of SNEC model adopts a rela-tivistic mean field equation of state with density-dependent couplings(HS (DD2). EOS). HS(DD2). EOS’s material phase divids into homogeneous nuclear matter and non-uniform nuclear matter. Homogeneous nuclear matter is used by Relativistic mean-field theory Non-uniform nuclear matter is used by Thomas-Fermi approximation. The progenitor star model of Woosley and Heger is used as the initial data for simulated calculation in this work. The progenitor star model taken as comparison is the 11.2M0. Sonic point position, density, temperature, symmetry energy, electronic abundance and lepton abundance are compared by both results from two numerical simulations. For equations of state of Wgxnu model Wangl and Wang2, there exist mutations in temperature, electronic abundance a-long with slight oscillations of lepton abundance in the interior of the star, but for equation of state of the SNEC model(HS (DD2). EOS), the stellar evolution is relatively stable. In order to rule the contingency of the above situation,we also calculate a number of progeni-tor star models as follow:11.4M☉、12M☉、13M☉、14M☉、15M☉、16M☉、17M☉、18M☉、 19M☉、21M☉、26M☉、27☉、28M☉、29M☉、30M☉、31M☉、50M☉、55M☉。The result-s show that the star have the mutations about the temperature,electronic abundance and abundance neutrinos. It could produce an inner shell in the iron core,which make a higher temperature in a supernova and make more drastic nuclear reaction,which can produce the phenomenon such as convection or fluctuation.