arXiv 1409.71742014-09hep-phastro-ph.GA

耗散暗扇区暗物质

Dissipative hidden sector dark matter

R. Foot, S. Vagnozzi

备注：: Some adjustments, 40 pages, 8 figures
发表信息：: Phys. Rev. D 91 (2015) 023512
DOI：: 10.1103/PhysRevD.91.023512

摘要：

在不修改已知的标准模型物理学的情况下解释暗物质的一个简单方法是要求存在一个隐藏的（暗）扇区，它主要通过引力与可见扇区相互作用。我们考虑一个隐藏的部门包含两个稳定的粒子下的一个完整的$U(1)^{'}$规范对称性，因此具有耗散的相互作用。与这种对称性相关的无质量规范场，即暗光子，可以通过动力学混合与普通光子相互作用。事实上，为了解释银河系的结构，这种$ε\sim 10 ^{-9}$强度的相互作用似乎是必要的。我们计算了这一新物理对大爆炸核合成的影响及其对氢复合时相对论能量密度的贡献。然后，我们研究了暗复合的过程，在此过程中形成的中性暗态，这是重要的大尺度结构的形成。接下来要讨论的是星系结构，重点是螺旋星系和不规则星系。对于这些星系，我们模拟的暗物质晕（在当前的时代）作为一个耗散等离子体的暗物质粒子，其中的能量损失，由于耗散是由普通超新星产生的能量补偿（核心崩溃的能量转移到隐藏的部门通过动力学混合诱导过程中的超新星核心）。我们发现，这样一个动力学晕模型可以再现盘星系的几个观察到的功能，包括核心的密度分布和塔利-费舍尔关系。我们还讨论了如何椭圆和矮球状星系可以适合这张照片。最后，这些分析相结合，我们的模型，这可以作为一个指导方针，为今后的实验搜索的参数空间设置界限。

英文摘要：

A simple way of explaining dark matter without modifying known Standard Model physics is to require the existence of a hidden (dark) sector, which interacts with the visible one predominantly via gravity. We consider a hidden sector containing two stable particles charged under an unbroken $U(1)^{'}$ gauge symmetry, hence featuring dissipative interactions. The massless gauge field associated with this symmetry, the dark photon, can interact via kinetic mixing with the ordinary photon. In fact, such an interaction of strength $ε\sim 10 ^{-9}$ appears to be necessary in order to explain galactic structure. We calculate the effect of this new physics on Big Bang Nucleosynthesis and its contribution to the relativistic energy density at Hydrogen recombination. We then examine the process of dark recombination, during which neutral dark states are formed, which is important for large-scale structure formation. Galactic structure is considered next, focussing on spiral and irregular galaxies. For these galaxies we modelled the dark matter halo (at the current epoch) as a dissipative plasma of dark matter particles, where the energy lost due to dissipation is compensated by the energy produced from ordinary supernovae (the core-collapse energy is transferred to the hidden sector via kinetic mixing induced processes in the supernova core). We find that such a dynamical halo model can reproduce several observed features of disk galaxies, including the cored density profile and the Tully-Fisher relation. We also discuss how elliptical and dwarf spheroidal galaxies could fit into this picture. Finally, these analyses are combined to set bounds on the parameter space of our model, which can serve as a guideline for future experimental searches.

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