2 research outputs found
Neutron stars and strange stars in the chiral SU(3) quark mean field model
We investigate the equations of state for pure neutron matter and strange
hadronic matter in -equilibrium, including , and
hyperons. The masses and radii of pure neutron stars and strange hadronic stars
are obtained. For a pure neutron star, the maximum mass is about , while for a strange hadronic star, the maximum mass is
around . The typical radii of pure neutron stars and
strange hadronic stars are about 11.0-12.3 km and 10.7-11.7 km, respectively.Comment: 18 pages, 7 figure
Effect of isovector-scalar meson on neutron star matter in strong magnetic fields
We study the effects of isovector-scalar meson on the equation of
state (EOS) of neutron star matter in strong magnetic fields. The EOS of
neutron-star matter and nucleon effective masses are calculated in the
framework of Lagrangian field theory, which is solved within the mean-field
approximation. From the numerical results one can find that the -field
leads to a remarkable splitting of proton and neutron effective masses. The
strength of -field decreases with the increasing of the magnetic field
and is little at ultrastrong field. The proton effective mass is highly
influenced by magnetic fields, while the effect of magnetic fields on the
neutron effective mass is negligible. The EOS turns out to be stiffer at G but becomes softer at stronger magnetic field after including the
-field. The AMM terms can affect the system merely at ultrastrong
magnetic field(G). In the range of G -- G the
properties of neutron-star matter are found to be similar with those without
magnetic fields.Comment: 26 pages, 9 figure