Magnetic Dual Chiral Density Wave: A Candidate Quark Matter Phase for the Interior of Neutron Stars
Magnetic Dual Chiral Density Wave: A Candidate Quark Matter Phase for the Interior of Neutron Stars
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DOI：
10.3390/universe7120458
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发表时间：
2021-11
期刊：
影响因子：
2.9
通讯作者：
E. J. Ferrer;V. de la Incera
中科院分区：
文献类型：
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作者：
E. J. Ferrer;V. de la Incera
在这篇综述中，我们讨论了致密夸克物质的磁双手征密度波（MDCDW）相的物理特性，并讨论了为什么它是一个有希望的候选者的内部物质相的中子星。MDCDW凝聚体在磁场存在下发生。它是一种单调制的手征密度波，其特征在于两个动态产生的参数：费米子准粒子质量m和凝聚空间调制q。MDCDW系统中的最低朗道能级准粒子模关于零能量是不对称的，这一事实导致了该相的拓扑性质和异常电输运。拓扑结构使得MDCDW相位对热声子波动具有鲁棒性，因此，它不会显示Landau-Peierls不稳定性，这是三维单调制非均匀手性凝聚体的主要特征。拓扑结构也反映在存在的电磁手征异常的有效行动和形成的杂交传播模式称为轴子极化激元。考虑到这个夸克相位的轴子极化激元之一是带隙的，我们讨论了如何入射γ射线光子可以转换成带隙的轴子极化激元在内部的磁星星星在MDCDW阶段导致星星崩溃，这种现象可以用来解释所谓的失踪脉冲星在银河系中心的问题。
In this review, we discuss the physical characteristics of the magnetic dual chiral density wave (MDCDW) phase of dense quark matter and argue why it is a promising candidate for the interior matter phase of neutron stars. The MDCDW condensate occurs in the presence of a magnetic field. It is a single-modulated chiral density wave characterized by two dynamically generated parameters: the fermion quasiparticle mass m and the condensate spatial modulation q. The lowest-Landau-level quasiparticle modes in the MDCDW system are asymmetric about the zero energy, a fact that leads to the topological properties and anomalous electric transport exhibited by this phase. The topology makes the MDCDW phase robust against thermal phonon fluctuations, and as such, it does not display the Landau–Peierls instability, a staple feature of single-modulated inhomogeneous chiral condensates in three dimensions. The topology is also reflected in the presence of the electromagnetic chiral anomaly in the effective action and in the formation of hybridized propagating modes known as axion-polaritons. Taking into account that one of the axion-polaritons of this quark phase is gapped, we argue how incident γ-ray photons can be converted into gapped axion-polaritons in the interior of a magnetar star in the MDCDW phase leading the star to collapse, a phenomenon that can serve to explain the so-called missing pulsar problem in the galactic center.