The restriction of ${\sigma }^{\ast }$ and $\varphi$ on the protoneutron stars PSR J0348+0432

Abstract

The restriction of ${\sigma }^{\ast }$ and $\varphi$ on the protoneutron star (PNS) PSR J0348+0432 is described by the relativistic mean field theory (RMFT) through choosing the effective coupling constants. We use an entropy per baryon S=1 to describe thermal effect on PSR J0348+0432 in this work and compare the differences between PNS PSR J0348+0432 with ${\sigma }^{\ast }$,$\varphi$ and without ${\sigma }^{\ast }$,$\varphi$. These effects include the particle number distribution, the mass-radius relation, the moment of inertia and the surface gravitational redshift. The PNS PSR J0348+0432 with ${\sigma }^{\ast }$ and $\varphi$ has more nucleons and will pushed forward the threshold for the appearance of the hyperons. The mass-radius relations are ($2.010M_{\odot }$,12.6520km) with ${\sigma }^{\ast }$ and $\varphi$ and ($2.010M_{\odot }$,12.6170km) without ${\sigma }^{\ast }$ and $\varphi$ respectively. The moment of inertia corresponding PNS PSR J0348+0432 are ($2.010M_{\odot }$,1.510$\times 10^{45}$g.cm${}^2$) and ($2.010M_{\odot }$,1.559$\times 10^{45}$g.cm${}^2$) respectively, the surface gravitational redshift corresponding PNS PSR J0348+0432 are ($2.010M_{\odot }$,0.3747) and ($2.010M_{\odot }$,0.3701) respectively. With the help of these calculations, we study the restriction of ${\sigma }^{\ast }$ and $\varphi$ on the interactions between baryons in PNS core.