An effective equation of state for dense matter with strangeness
- 作者：Balberg ; Shmuel ; Gal ; Avraham
- 关键词：21.30.Fe ; 26.60.+c ; 97.60.BW ; 97.60.Jd ; Equation of state ; Effective interactions ; Strangeness in neutron stars
- 刊名：Nuclear Physics A
- 出版年：1997
- 期刊代码：44_03759474
- 类别：ph
- 出版时间：October 27, 1997
- 卷：625
- 期：1-2
- 页码：435-472
- 文件大小：2.05 M
摘要
An effective equation of state which generalizes the Lattimer-Swesty equation for nuclear matter is presented for matter at supernuclear densities including strange baryons. It contains an adjustable baryon potential energy density, based on models of local potentials for the baryon-baryon interactions. The features of the equation rely on the properties of nuclei for the nucleon-nucleon interactions, and mainly on experimental data from hypernuclei for the hyperon-nucleon and hyperon-hyperon interactions. The equation is used to calculate equilibrium compositions and thermodynamic properties of high density matter with strangeness in two astrophysical contexts: neutron star matter (transparent to neutrinos) and proto-neutron star matter (opaque to neutrinos). The effective equation of state reproduces typical properties of high density matter found in theoretical microscopic models. Of these, the main result is that hyperons appear in both types of matter at about twice the nuclear saturation density, and that their appearance significantly softens the equation of state. The range of maximal masses of neutron stars found in a comprehensive parameter survey is 1.4-1.7M
. Another typical result is that the maximal mass of a proto-neutron star with strange baryons is higher than that of an evolved neutron star (opposite to the case of nuclear matter), setting the stage for a “delayed collapse” scenario.
. Another typical result is that the maximal mass of a proto-neutron star with strange baryons is higher than that of an evolved neutron star (opposite to the case of nuclear matter), setting the stage for a “delayed collapse” scenario.