超子相互作用與中子星性質(zhì)-資料下載頁
2025-08-01 14:11本頁面
【正文】 ??=1????epn?i/?? (f m3)0 .0 0 .2 0 .4 0 .6 0 .81 E41 E30 .0 10 .11C ASE 2 , x??=1?? ??epn?i/??B (f m)0 .0 0 .2 0 .4 0 .6 0 .81 E41 E30 .0 10 .11C ASE 3 , x??=1???epn?i/??B (f m)Particle fraction as a function of baryon density for different Cases Scalar meson interaction effect The Sigama is absent because of the strong repulsion The Cascade starts appearing at high density due to less attraction 1 4 .2 1 4 .4 1 4 .6 1 4 .8 1 5 .0 1 5 .2 1 5 .4 1 5 .60 .00 .20 .40 .60 .81 .01 .21 .41 .6 ca se 1 ca se 2 ca se 3 ca se 4Mm a x= 5 f o r ca se 1 = 1 .4 3 0 f o r c a s e 2 = 1 .3 9 6 f o r c a s e 3 = 1 .4 5 9 f o r c a s e 4 = 1 .9 3 2 f o r o n l y NM/Msunl o g ( ?c) (g / cm3)gravitation mass as a function of central energy density for different cases Hyperons significantly reduce maximum neutron star mass from to . However, the change in maximum mass limit is insignificant against different hyperon scalar couplings. In all cases, the mass are in recent observational limit(Phys. Rep.,328(2022)237 ). ⊙⊙Summary In the strange baryons sector,we considered different hyperon Couplings from the analysis of various experiment data and found: The sigma hyperons are absent in the neutron star matter,when these experience strong repulsive force and isospin interaction These different uncertainties of hyperon couplings do not change the maximum mass of the neutron star significantly Thank you
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