English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present sets of equation of state (EOS) of nuclear matter includinghyperons using an SU_f(3) extended relativistic mean field (RMF) model with awide coverage of density, temperature, and charge fraction for numericalsimulations of core collapse supernovae. Coupling constants of Sigma and Xihyperons with the sigma meson are determined to fit the hyperon potentialdepths in nuclear matter, U_Sigma(rho_0) ~ +30 MeV and U_Xi(rho_0) ~ -15 MeV,which are suggested from recent analyses of hyperon production reactions. Atlow densities, the EOS of uniform matter is connected with the EOS by Shen etal., in which formation of finite nuclei is included in the Thomas-Fermiapproximation. In the present EOS, the maximum mass of neutron stars decreasesfrom 2.17 M_sun (Ne mu) to 1.63 M_sun (NYe mu) when hyperons are included. In aspherical, adiabatic collapse of a 15$M_\odot$ star by the hydrodynamicswithout neutrino transfer, hyperon effects are found to be small, since thetemperature and density do not reach the region of hyperon mixture, where thehyperon fraction is above 1 % (T > 40 MeV or rho_B > 0.4 fm^{-3}).

Tables of Hyperonic Matter Equation of State for Core-Collapse Supernovae