Influence of Entropy on Composition and Structure of Massive Protoneutron Stars
| Autor: | Bin Hong, X. X. Zhou, Huan-Yu Jia, Xue-Ling Mu |
|---|---|
| Rok vydání: | 2016 |
| Předmět: |
Physics
Coupling constant Physics and Astronomy (miscellaneous) 010308 nuclear & particles physics Astrophysics::High Energy Astrophysical Phenomena Nuclear Theory Hyperon Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Moment of inertia 01 natural sciences Baryon Stars Neutron star 0103 physical sciences Energy density 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics Gravitational redshift |
| Zdroj: | Communications in Theoretical Physics. 66:224-230 |
| ISSN: | 0253-6102 |
| DOI: | 10.1088/0253-6102/66/2/224 |
| Popis: | Adjusting the suitable coupling constants in relativistic mean Geld (RMF) theory and focusing on thermal effect of an entropy per baryon (S) from 0 to 3, we investigate the composition and structure of massive protoneutron stars corresponding PSR J1614-2230 and PSR J0348+0432. It is found that massive protoneutron stars (PNSs) have more hyperons than cold neutron stars. The entropy per baryon will stiffen the equation of state, and the influence on the pressure is more obvious at low density than high density, while the influence on the energy density is more obvious at high density than low density. It is found that higher entropy will give higher maximum mass, higher central temperature and lower central density. The entropy per baryon changes from 0 to 3, the radius of a PNS corresponding PSR J0348+0432 will increase from 12.86 km to 19.31 km and PSR J1612-2230 will increase from 13.03 km to 19.93 km. The entropy per baryon will raise the central temperature of massive PNSs in higher entropy per baryon, but the central temperature of massive PNSs maybe keep unchanged in lower entropy per baryon. The entropy per baryon will increase the moment of inertia of a massive protoneutron star, while decrease gravitational redshift of a massive neutron star. |
| Databáze: | OpenAIRE |
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