中文摘要：

We study the properties of dense matter at finite temperature with various proton fractions for use in supernova simulations.The relativistic mean-field theory is used to describe homogeneous nuclear matter,while the Thomas-Fermi approximation is adopted to describe inho-mogeneous matter.We also discuss the equation of state of neutron star matter at zero tempera-ture in a wide density range.The equation of state at high densities can be significantly softened by the inclusion of hyperons.

英文摘要：

We study the properties of dense matter at finite temperature with various proton fractions for use in supernova simulations. The relativistic mean-field theory is used to describe homogeneous nuclear matter, while the Thomas-Fermi approximation is adopted to describe inhomogeneous matter. We also discuss the equation of state of neutron star matter at zero temperature in a wide density range. The equation of state at high densities can be significantly softened by the inclusion of hyperons.