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Wave Dark Matter
Annual Review of Astronomy and Astrophysics ( IF 26.3 ) Pub Date : 2021-09-08 , DOI: 10.1146/annurev-astro-120920-010024
Lam Hui 1
Affiliation  

We review the physics and phenomenology of wave dark matter: a bosonic dark matter candidate lighter than about 30 eV. Such particles have a de Broglie wavelength exceeding the average interparticle separation in a galaxy like the Milky Way and are, thus, well described as a set of classical waves. We outline the particle physics motivations for such particles, including the quantum chromodynamics axion as well as ultralight axion-like particles such as fuzzy dark matter. The wave nature of the dark matter implies a rich phenomenology:

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Wave interference gives rise to order unity density fluctuations on de Broglie scale in halos. One manifestation is vortices where the density vanishes and around which the velocity circulates. There is one vortex ring per de Broglie volume on average.

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For sufficiently low masses, soliton condensation occurs at centers of halos. The soliton oscillates and undergoes random walks, which is another manifestation of wave interference. The halo and subhalo abundance is expected to be suppressed at small masses, but the precise prediction from numerical wave simulations remains to be determined.

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For ultralight ∼10−22 eV dark matter, the wave interference substructures can be probed by tidal streams or gravitational lensing. The signal can be distinguished from that due to subhalos by the dependence on stream orbital radius or image separation.

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Axion detection experiments are sensitive to interference substructures for wave dark matter that is moderately light. The stochastic nature of the waves affects the interpretation of experimental constraints and motivates the measurement of correlation functions.



中文翻译:

波暗物质

我们回顾了波暗物质的物理学和现象学:一种比约 30 eV 轻的候选玻色暗物质。这种粒子的德布罗意波长超过了银河系这样的星系中的平均粒子间距,因此被很好地描述为一组经典波。我们概述了此类粒子的粒子物理学动机,包括量子色动力学轴子以及超轻轴子状粒子,如模糊暗物质。暗物质的波动性意味着丰富的现象学:

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波干涉在光晕中引起德布罗意尺度上的有序单位密度波动。一种表现形式是密度消失且速度在其周围循环的涡流。每个德布罗意体积平均有一个涡环。

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对于足够低的质量,孤子凝聚发生在晕的中心。孤子振荡并进行随机游走,这是波干涉的另一种表现形式。晕和亚晕的丰度预计在小质量时会受到抑制,但数值波模拟的精确预测仍有待确定。

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对于超轻~10 -22 eV 暗物质,波干涉子结构可以通过潮汐流或引力透镜探测。通过依赖于流轨道半径或图像分离,可以将信号与由亚晕引起的信号区分开来。

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轴子探测实验对中等亮度的波暗物质的干涉子结构敏感。波的随机性影响实验约束的解释并激发相关函数的测量。

更新日期:2021-09-09
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