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Antikaon Condensation and In-medium Kaon and Antikaon Production in Protoneutron Stars

Communications in Theoretical Physics 2007年第1期47卷 111-118页

作者： GU Jian-Fa GUO Hua LI Xi-Guo LIU Yu-Xin XU Fu-Rong Department of Technical Physics and MOE Laboratory of Heavy Ion Physics Peking University Beijing 100871 China Center of Theoretical Nuclear Physics National Laboratory of Heavy Ion Accelerator Lanzhou 730000 China Institute of Modern Physics The Chinese Academy of Sciences Lanzhou 730000 China Department of Physics Peking University Beijing 100871 China

Antikaon condensation and kaon and antikaon production in protoneutron stars are investigated in a chiral hadronic model （also referred to as the FST model in this paper）. The effects of neutrino trapping on protoneutron stars are analyzed systematically. It is shown that neutrino trapping makes the critical density of K^- condensation delay to higher density and fifo condensation not occur. The equation of state （EOS） of （proto）neutron star matter with neutrino trapping is stiffer than that without neutrino trapping. As a result, the maximum masses of （proto）neutron stars with neutrino trapping are larger than those without neutrino trapping. If hyperons are taken into account, antikaon does not form a condensate 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. Finally, our results illustrate that the Q values for K^＋ and K^- production in （proto）neutron stars are not sensitive to neutrino trapping and inclusion of hyperons.

关键词： protoneutron stars antikaon condensation neutrino trapping

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Deconfinement Phase Transition Including Perturbative QCD Corrections in (Proto)neutron Star Matter

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Communications in Theoretical Physics 2008年第2期49卷 461-466页

作者： GU Jian-Fa GUO Hua LEE Xi-Guo LIU Yu-Xin XU Fu-Rong Department of Technical Physics and MOE Laboratory of Heavy Ion Physics Peking University Beijing 100871 China Center of Theoretical Nuclear Physics National Laboratory of Heavy Ion Accelerator Lanzhou 730000 China Institute of Modern Physics The Chinese Academy of Sciences Lanzhou 730000 China Department of Physics Peking University Beijing 100871 China

Deconlinement phase transition and neutrino trapping in （proto）neutron star matter are investigated in a chiral hadronic model （also referred to as the FST model） for the hadronic phase （HP） and in the color-flavor-locked （CFL） quark model for the deconlined quark phase. We include a perturbative QCD correction parameter αs in the CFL quark matter equation of states. It is shown that the CFL quark core with K^0 condensation forms in neutron star matter with the large value of αs. If the small value of αs is taken, hyperons suppress the CFL quark phase and the liP is dominant in the high-density region of （proto）neutron star matter. neutrino trapping makes the fraction of the CFL quark matter decrease compared with those without neutrino trapping. Moreover, increasing the QCD correction parameter as or decreasing the bag constant B and the strange quark mass ms can make the fraction of the CFL quark matter increase, simultaneously, the fraction of neutrino in protoneutron star matter increases, too. The maximum masses and the corresponding radii of （proto）neutron stars are not sensitive to the QCD correction parameter αs.

关键词： deconfinement phase transition neutrino trapping neutron star matter

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