2018/04/10 by Bin Hong, Zhong-Zhou Ren
Physics and Astronomy · #Astrophysical Phenomena and Observations #Baryon #Coupling (piping) #Moment of inertia #Pulsars and Gravitational Waves Research #Redshift #Star (game theory) #Stellar, planetary, and galactic studies #Thermal #nucl-th
paper · pdf · doi:10.1088/1674-1137/42/8/084105
arxiv created 2018/04/10 · openalex created_date 2018/04/24 · openalex publication_date 2018/07/01 · arxiv updated 2018/08/15 · openalex updated_date 2026/08/05
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 (2.010 M ⊙ , 12.6520 km) with σ* and ϕ and (2.010 M ⊙ , 12.6170 km) without σ* and ϕ. The moments of inertia corresponding to PNS PSR J0348+0432 are (2.010 M ⊙ , 1.510 × 10 45 g·cm 2 ) and (2.010 M ⊙ , 1.559 × 10 45 g·cm 2 ) respectively, and the surface gravitational redshifts are (2.010 M ⊙ , 0.3747) and (2.010 M ⊙ , 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.