反馈能解决大到不能倒的问题吗？
Can Feedback Solve the Too Big to Fail Problem?
摘要：
观测到的银河系矮球状星系（dSphs）的中心密度显着低于在银河系大小的暗物质主机的无耗散模拟中发现的最大（Vmax约35公里/秒）的subhalos的密度。一个可能的解释是，从反馈中去除气体可以降低核心密度，足以与观测结果相匹配。我们通过在高分辨率，理想化的数值模拟中使用随时间变化的中心势来模拟超新星反馈的动力学效应，并探索由此产生的对矮暗物质晕质量分布的影响。我们发现，为了使M星的中心质量与观测到的10^6 M太阳dSphs相匹配，必须以100%的效率将40，000多颗超新星的能量当量直接传递到暗物质。这个能量需求超过了在大多数dSphs中爆炸的超新星的数量，对于典型的初始质量函数。我们还发现，每单位的能量传递和每累积质量从星系中删除，单一的吹出事件是更有效地减少中央暗物质密度比重复的小爆发。我们的结论是，这是不可能的超新星反馈单独可以解决银河系subhalos的“太大而不能倒”的问题。
英文摘要：
The observed central densities of Milky Way dwarf spheroidal galaxies (dSphs) are significantly lower than the densities of the largest (Vmax about 35 km/s) subhalos found in dissipationless simulations of Galaxy-size dark matter hosts. One possible explanation is that gas removal from feedback can lower core densities enough to match observations. We model the dynamical effects of supernova feedback through the use of a time-varying central potential in high resolution, idealized numerical simulations and explore the resulting impact on the mass distributions of dwarf dark matter halos. We find that in order to match the observed central masses of M_star about 10^6 M_sun dSphs, the energy equivalent of more than 40,000 supernovae must be delivered with 100% efficiency directly to the dark matter. This energy requirement exceeds the number of supernovae that have ever exploded in most dSphs for typical initial mass functions. We also find that, per unit energy delivered and per cumulative mass removed from the galaxy, single blow-out events are more effective than repeated small bursts in reducing central dark matter densities. We conclude that it is unlikely that supernova feedback alone can solve the "Too Big to Fail" problem for Milky Way subhalos.
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