耗散暗物质晕：稳态解II
Dissipative dark matter halos: The steady state solution II
摘要：
在镜像暗物质模型和一般的耗散暗物质模型中，具有活跃恒星形成的星系（包括螺旋星系和富含气体的矮星）周围的晕是动态的：它们响应于加热和冷却过程而膨胀和收缩。普通的II型超新星（SN）可以提供主要的热源，如果动力学混合相互作用存在强度为$ε\sim 10^{-9} - 10^{-10}$的话。耗散的暗物质晕可以被模拟为由欧拉方程控制的流体。在足够孤立和不受扰动的星系周围，晕可以放松到一个稳定状态的配置，在那里加热和冷却速率局部平衡和流体静力学平衡占上风。这些稳定状态的条件，可以解决导出的物理性质，包括晕密度和温度分布，模型星系。在这里，我们考虑了镜面暗粒子模型中的理想球对称星系，如早期论文[论文I，arXiv：1707.02528]所述，但我们假设SN附近的局部晕加热比辐射源占主导地位。有了这个假设，物理上有趣的稳定状态的解决方案出现，我们计算的模型星系的代表性范围。最终的结果是一个相当简单的描述暗物质晕周围的理想化球对称系统，其特点是原则上只有一个参数，与物理性质非常相似的经验性质的磁盘星系。
英文摘要：
Within the mirror dark matter model and dissipative dark matter models in general, halos around galaxies with active star formation (including spirals and gas rich dwarfs) are dynamical: they expand and contract in response to heating and cooling processes. Ordinary Type II supernovae (SN) can provide the dominant heat source, possible if kinetic mixing interaction exists with strength $ε\sim 10^{-9} - 10^{-10}$. Dissipative dark matter halos can be modelled as a fluid governed by Euler's equations. Around sufficiently isolated and unperturbed galaxies the halo can relax to a steady state configuration, where heating and cooling rates locally balance and hydrostatic equilibrium prevails. These steady state conditions can be solved to derive the physical properties, including the halo density and temperature profiles, for model galaxies. Here, we have considered idealized spherically symmetric galaxies within the mirror dark particle model, as in the earlier paper [paper I, arXiv:1707.02528], but we have assumed that the local halo heating in the SN vicinity dominates over radiative sources. With this assumption, physically interesting steady state solutions arise which we compute for a representative range of model galaxies. The end result is a rather simple description of the dark matter halo around idealized spherically symmetric systems, characterized in principle by only one parameter, with physical properties that closely resemble the empirical properties of disk galaxies.
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