Camouflage of the Phase Transition to Quark Matter in Neutron Stars
Camouflage of the Phase Transition to Quark Matter in Neutron Stars
复制标题
中子星中夸克物质相变的伪装
DOI：
10.3847/1538-4357/ab53ea
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发表时间：
2018-11
期刊：
影响因子：
--
通讯作者：
Prashanth Jaikumar
中科院分区：
文献类型：
--
作者：
Wei Wei;Bryen Irving;Marc Salinas;Thomas Klähn;Prashanth Jaikumar
一段时间以来，人们已经知道含有夸克物质的致密恒星可以在测量的质量和半径范围内伪装成中子星，这使得很难对星星内部物质的相态得出确切的结论。使用矢量增强袋模型（vBag），我们研究质量半径和质量紧关系与麦克斯韦和吉布斯建设的混合星与过渡从核物质到两个或三个味夸克物质，包括顺序过渡。稳定的混合星不仅可以用两味或三味夸克物质来模仿中子星（传统的伪装），而且似乎很难区分两味和三味夸克物质，即使在可以说已经发生相变的情况下，例如在质量-半径关系中存在明显的扭结。此外，考虑到连续的味道过渡，我们发现，过渡到一个不稳定的分支可以引起的过渡从核到不稳定的夸克物质或连续的过渡从核到稳定的，但"伪装"的二味到不稳定的三味夸克物质。像vBag一样，在相变模型中解决手征恢复和夸克解除禁闭，为高密度状态方程增加了进一步的灵活性，促使人们在使用高精度M-R数据时谨慎，以得出关于中子星中相和相变性质的明确结论。
It has been known for some time that compact stars containing quark matter can masquerade as neutron stars in the range of measured mass and radius, making it difficult to draw firm conclusions on the phases of matter present inside the star. Using the vector-enhanced Bag model (vBag), we examine mass–radius and mass–compactness relations with Maxwell and Gibbs construction for hybrid stars with transitions from nuclear matter to two- or three-flavor quark matter, including sequential transitions. Not only can stable hybrid stars with either two- or three-flavor quark matter mimic neutron stars (the traditional masquerade), it also appears difficult to distinguish two-flavor from three-flavor quark matter, even in cases where a phase transition can be said to have occurred, such as in the presence of a distinct kink in the mass–radius relation. Furthermore, allowing for sequential flavor transitions, we find that the transition into an unstable branch can be caused by either a transition from nuclear to unstable quark matter or the sequential transition from nuclear to stable but “masquerading” two-flavor to unstable three-flavor quark matter. Addressing chiral restoration as well as quark deconfinement in a model of the phase transition, as the vBag does, adds further flexibility to the high-density equation of state, motivating caution in using even high-precision M–R data to draw firm conclusions on the nature of phases and phase transitions in neutron stars.
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DOI：
10.1088/1742-6596/509/1/012075
发表时间：
2013-10
期刊：
Journal of Physics: Conference Series
影响因子：
--
作者：
Tomoki Endo
通讯作者：
Tomoki Endo
DOI：
10.1063/1.2714446
发表时间：
2007-02
期刊：
--
影响因子：
--
作者：
M. Buballa
通讯作者：
M. Buballa
影响因子：
5
作者：
M. Alford;Sophia Han;M. Prakash
通讯作者：
M. Alford;Sophia Han;M. Prakash
影响因子：
9.6
作者：
F. Weber
通讯作者：
F. Weber
影响因子：
5
作者：
Andreas Zacchi;Rainer Stiele;J. Schaffner-Bielich
通讯作者：
Andreas Zacchi;Rainer Stiele;J. Schaffner-Bielich