耗散暗物质晕：稳态解
Dissipative dark matter halos: The steady state solution
摘要：
耗散暗物质，其中暗物质粒子的性质非常类似于熟悉的重子物质，被认为是。镜像暗物质来自于一个同构的隐藏扇区，是一个特定的、理论上受限制的场景。其他的可能性包括具有更一般的隐藏扇区的模型，这些隐藏扇区包含无质量的暗光子（不间断的$U(1)$规范相互作用）。这种暗物质不仅具有耗散冷却过程，而且还被认为具有来自普通超新星的非平凡加热（由动力学混合相互作用促进）。旋转支撑星系周围的耗散暗物质晕的动力学，受加热和冷却过程的影响，可以用流体方程模拟。对于一个足够孤立的星系，稳定的恒星形成率，耗散的暗物质晕预计将演变到一个稳态的配置，这是在流体静力学平衡和加热和冷却速率局部平衡。在这里，我们考虑到主要的冷却和加热过程，并数值求解的稳定状态下的解决方案的假设球对称，可以忽略不计的暗磁场，和超新星源能量通过暗辐射传输到晕。对于所考虑的参数和所做的假设，我们无法找到一个物理上现实的解决方案，为约束情况下的镜像暗物质晕。在实际的晕圈质量密度下，晕圈冷却通常超过加热。这个问题可以在更一般的耗散暗物质模型中得到纠正，我们将详细讨论一个具体的例子。
英文摘要：
Dissipative dark matter, where dark matter particle properties closely resemble familiar baryonic matter, is considered. Mirror dark matter, which arises from an isomorphic hidden sector, is a specific and theoretically constrained scenario. Other possibilities include models with more generic hidden sectors that contain massless dark photons (unbroken $U(1)$ gauge interactions). Such dark matter not only features dissipative cooling processes, but is also assumed to have nontrivial heating sourced by ordinary supernovae (facilitated by the kinetic mixing interaction). The dynamics of dissipative dark matter halos around rotationally supported galaxies, influenced by heating as well as cooling processes, can be modelled by fluid equations. For a sufficiently isolated galaxy with stable star formation rate, the dissipative dark matter halos are expected to evolve to a steady state configuration which is in hydrostatic equilibrium and where heating and cooling rates locally balance. Here, we take into account the major cooling and heating processes, and numerically solve for the steady state solution under the assumptions of spherical symmetry, negligible dark magnetic fields, and that supernova sourced energy is transported to the halo via dark radiation. For the parameters considered, and assumptions made, we were unable to find a physically realistic solution for the constrained case of mirror dark matter halos. Halo cooling generally exceeds heating at realistic halo mass densities. This problem can be rectified in more generic dissipative dark matter models, and we discuss a specific example in some detail.
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