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An equilibrium dark matter halo with the Burkert profile

机译：具有Burkert轮廓的平衡暗物质晕

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摘要

In this paper a prescription for generating an equilibrium spherical system depicted with cuspy density profiles is extended to a core density profile, the Burkert profile, which is observationally more suitable to dwarfs. By using a time-saving Monte Carlo method instead of N-body simulations, we show that the Burkert halo, which is initialized with a distribution function that depends only on energy, is in a practically stable equilibrium. The one generated with the local Maxwellian approximation is unstable, where the flat core density structure tends to steepen. This is fundamentally different from a previous study on a halo with a cuspy density profile. The deviation of the unstable "Burkert" from the initial Burkert profile is found to be closely related to taking a Gaussian as the velocity distribution at any given point. The significance of not using the local Maxwellian approximation is further demonstrated by exploring the dynamical evolution of compact super star clusters (SSCs) in the Burkert halo. In particular, the local Maxwellian approximation results in underestimating the dynamical friction and overestimating sinking time scale. Accordingly, this leads to a lower probability of forming massive bulges and young nuclear star clusters in bulgeless galaxies.
机译：在本文中，用于生成具有尖细密度分布图的平衡球面系统的处方被扩展为核心密度分布图，即Burkert分布图，据观察，它更适合于侏儒。通过使用省时的蒙特卡洛方法而不是N体模拟，我们证明了Burkert晕实际上处于稳定的平衡状态，该Burkert晕使用仅取决于能量的分布函数进行了初始化。用局部麦克斯韦近似生成的一个是不稳定的，其中扁平的核密度结构趋于陡峭。这与先前关于具有密集密度分布的光晕的研究有根本的不同。发现不稳定的“ Burkert”与初始Burkert轮廓的偏差与在任何给定点采用高斯速度分布密切相关。通过探索Burkert晕中的紧凑型超级星团（SSC）的动力学演化，进一步证明了不使用局部麦克斯韦逼近的重要性。特别是，局部麦克斯韦近似值导致低估了动态摩擦力而高估了下沉时间尺度。因此，这会导致在较低的星系中形成大的凸起和年轻的核星团的可能性降低。

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