Potential Depth of Σ-hyperons in Saturated Nuclear Matter and Rotational Inertia of Proto Neutron Star†

In the framework of relativistic mean field theory and taking account of the baryon octet system {n, p,Λ,Σ−,Σ0,Σ+, Ξ−, Ξ0}, the influence of the potential depth U(N) Σ of Σ-hyperon in saturated nuclear matter on the rotational inertia of proto neutron star (PNS) is investigated. It is found that the rotational inertia corresponding to the maximum mass of PNS increases, respectively, by a factor of 0.44%, 0.29% and 0.08%, for the attractive potential depth U(N) Σ = -30 MeV, -20MeV, -10MeV and 0MeV, and increases by a factor of 0.06% and 0.08% for the repulsive potential depth U(N) Σ =  + 10MeV, + 20MeV and + 30 MeV. The effect of the attractive (negative) potential depth U(N) Σ on the rotational inertia corresponding to the maximum mass of PNS is several times larger than that of the repulsive (positive) one.     

Effects of α-Enhancement on Stellar Evolution

Using Eggleton's code, we systematically show the differences in stellar evolution between the results based on the scaled-solar mixture and the α-enhanced metal mixture. As input, the OPAL high temperature opacities are used for log (T/K)>4.00, and the new Wichita State low temperature opacities, for log (T/K)≤4.00. Our calculations cover star masses ranging from 0.25 to 80.0 M⊙, spaced at Δlog M=0.10 or 0.05. The values of metallicities Z are 0.0001, 0.0003, 0.001, 0.004, 0.01, 0.02, 0.03, 0.04, 0.06, 0.08 and 0.10. For a given Z, the initial hydrogen mass fraction is given by X=0.76-3.0Z. We show that α-enhancement can raise the stellar effective temperature and luminosity, and reduce the evolutionary age. Compared with some previous work, the effects of α-enhancement are more obviously demonstrated in our calculations.     

Rotation Profiles of Solar-like Stars with Magnetic Fields

We investigate the rotation profile of solar-like stars with magnetic fields. A diffu-sion coefficient of magnetic angular momentum transport is deduced. Rotating stellar models with different mass incorporating the coefficient are computed to give the rotation profiles. The total angular momentum of a solar model with only hydrodynamic instabilities is about 13 times larger than that of the Sun at the age of the Sun, and this model can not reproduce quasi-solid rotation in the radiative region. However, the solar model with magnetic fields not only can reproduce an almost uniform rotation in the radiative region, but also a total angular momentum that is consistent with the helioseismic result at the 3 σ level at the age of the Sun. The rotation of solar-like stars with magnetic fields is almost uniform in the radiative region, but for models of 1.2-1.5 M⊙, there is an obvious transition region between the convective core and the radiative region, where angular velocity has a sharp radial gradient, which is different from the rotation profile of the Sun and of massive stars with magnetic fields. The change of angular velocity in the transition region increases with increasing age and mass.