Antikaon Condensation and Hyperons Production in Protoneutron Stars

GU Jian-fa; GUO Hua; LI Xiguo; LIU Yu-xin

doi:10.11804/NuclPhysRev.22.04.429

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Article Navigation > Nuclear Physics Review > 2005 > 22(4): 429-433

GU Jian-fa, GUO Hua, LI Xiguo, LIU Yu-xin, . Antikaon Condensation and Hyperons Production in Protoneutron Stars[J]. Nuclear Physics Review, 2005, 22(4): 429-433. doi: 10.11804/NuclPhysRev.22.04.429

Citation:

GU Jian-fa, GUO Hua, LI Xiguo, LIU Yu-xin, . Antikaon Condensation and Hyperons Production in Protoneutron Stars[J]. Nuclear Physics Review, 2005, 22(4): 429-433. doi: 10.11804/NuclPhysRev.22.04.429

Antikaon Condensation and Hyperons Production in Protoneutron Stars

doi: 10.11804/NuclPhysRev.22.04.429

1 Department of Technical Physics, and MOE Laboratory of Heavy Ion Physics, Peking University, Beijing 100871, China; 2 Center of Theoretical Nuclear Physics, National Laboratory of Heavy Accelerator of Lanzhou, Lanzhou 730000, China; 3 Department of Physics, Peking University, Beijing 100871, China

Received Date: 1900-01-01
Rev Recd Date: 1900-01-01
Publish Date: 2005-12-20

Abstract

A chiral hadronic model is extended to investigate antikaon condensation and hyperons production of protoneutron stars. Our results show that neutrino trapping makes the critical density of K^- condensation delay to higher density and K^-0 condensation not occur. Meanwhile, the equation of state （EOS） of （proto）neutron star matter considering neutrino trapping is stiffer than the case without neutrino trapping. Therefore the maximum masses of rotoneutron stars with neutrino trapping are larger than those without neutrino trapping. If hyperons are considered, antikaon condensation does not appear in （proto） neutron stars. Meanwhile, the corresponding EOS becomes much softer, and the maximum masses of （proto）neutron stars are smaller than those without hyprons.
- chiral hadronic model,
- antikaon condensation,
- protoneutron star
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Antikaon Condensation and Hyperons Production in Protoneutron Stars

doi: 10.11804/NuclPhysRev.22.04.429

1 Department of Technical Physics, and MOE Laboratory of Heavy Ion Physics, Peking University, Beijing 100871, China; 2 Center of Theoretical Nuclear Physics, National Laboratory of Heavy Accelerator of Lanzhou, Lanzhou 730000, China; 3 Department of Physics, Peking University, Beijing 100871, China

Received Date: 1900-01-01
Rev Recd Date: 1900-01-01
Publish Date: 2005-12-20

Key words:

Abstract: A chiral hadronic model is extended to investigate antikaon condensation and hyperons production of protoneutron stars. Our results show that neutrino trapping makes the critical density of K^- condensation delay to higher density and K^-0 condensation not occur. Meanwhile, the equation of state （EOS） of （proto）neutron star matter considering neutrino trapping is stiffer than the case without neutrino trapping. Therefore the maximum masses of rotoneutron stars with neutrino trapping are larger than those without neutrino trapping. If hyperons are considered, antikaon condensation does not appear in （proto） neutron stars. Meanwhile, the corresponding EOS becomes much softer, and the maximum masses of （proto）neutron stars are smaller than those without hyprons.

GU Jian-fa, GUO Hua, LI Xiguo, LIU Yu-xin, . Antikaon Condensation and Hyperons Production in Protoneutron Stars[J]. Nuclear Physics Review, 2005, 22(4): 429-433. doi: 10.11804/NuclPhysRev.22.04.429

Citation: