Abstract
The influence of σ* and ϕ on the proto-neutron star (PNS) PSR J0348+0432 is described by the relativistic mean field theory (RMFT) through choosing effective coupling constants. We use an entropy per baryon S = 1 to describe the thermal effects on PSR J0348+0432 in this work and compare this PNS with and without σ*, ϕ. These effects include the particle number distribution, mass-radius relation, moment of inertia and surface gravitational redshift. The PNS PSR J0348+0432 with σ* and ϕ has more nucleons and will push forward the threshold for the appearance of the hyperons. The mass-radius relations are (2.010M ⊙, 12.6520 km) with σ* and ϕ and (2.010M ⊙, 12.6170 km) without σ* and ϕ. The moments of inertia corresponding to PNS PSR J0348+0432 are (2.010M ⊙, 1.510 × 1045 g·cm2) and (2.010M ⊙, 1.559 × 1045 g·cm2) respectively, and the surface gravitational redshifts are (2.010M ⊙, 0.3747) and (2.010M ⊙, 0.3701) respectively. With the help of these calculations, we study the restriction of σ* and ϕ on the interactions between baryons in the PNS core.
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