Deconfinement Phase Transition Including Perturbative QCD Corrections in (Proto)neutron Star Matter
Deconfinement Phase Transition Including Perturbative QCD Corrections in (Proto)neutron Star Matter
复制标题
解禁闭相变，包括（原）中子星物质中的微扰 QCD 校正
DOI：
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发表时间：
2008
期刊：
影响因子：
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通讯作者：
Xu Fu
中科院分区：
文献类型：
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作者：
Gu Jianfa;Guo Hua;Lee Xiguo;Liu Yu;Xu Fu
用强子相（HP）的手性强子模型（也称为FST模型）和色香味锁定夸克相（CFL）夸克模型研究了（原）中子星物质中的非约束相变和中微子捕获。我们在CFL夸克物质状态方程中加入了一个微扰QCD校正参数αs。结果表明，在αs值较大的中子星物质中可以形成K0凝聚的CFL夸克核。如果αs值较小，则超子抑制CFL夸克相，HP在（原）中子星物质的高密度区占主导地位。中微子捕获使得CFL夸克物质的比例比没有中微子捕获的夸克物质的比例降低。此外，增大QCD校正参数αs或减小袋常数B和奇异夸克质量ms可使CFL夸克物质的比例增大，同时质子中子星物质中中微子的比例也增大。（原）中子星的最大质量和相应半径对QCD校正参数αs不敏感。
Deconfinement 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 deconfined 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 K0 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 HP 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 αs 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.