宇宙学年龄上小H2团簇中中性伴子产生重子
Producing baryons from neutralinos in small H2 clumps over cosmological ages
摘要：
类星体中的极端散射事件表明存在质量为$\rm \sim 10^{-3} M_\odot$、大小为$\rm \sim 10 AU$的暗$\rm H_2 $团块。与通过N体模拟获得的相同质量的WIMP团块相比，这样的团块是极其密集的。一个被中心$\rm H_2 $团引力吸引的WIMP团将经历第一次下降，在此期间，它的密度增加了$\rm \sim 1 Myr$中的$\rm 10^6$。在这张海报中，我开始探索由$\rm H_2 $和WIMP制成的混合团块的现象学。由团块构成的分子云是将WIMP的平滑分布转化为密集网络的有效机器。如果WIMP是被引力吸引在这种分子云团块中的中性伴子，它们可能会在宇宙学年龄内富集重子扇区，或者与冷的$\rm H_2 $云混合，直到团块因碰撞或恒星紫外线加热而蒸发。一个唯象模型的基础上假设的黑暗重子组件（DBC），在过去被调用来解释CDM配置文件的主要缺点之一，其过于密集的核心，在这方面进行了简要的回顾。DBC被$\rm H_2 $和WIMP的混合物所取代，其中一小部分HI是由内部$\rm H_2 $碰撞产生的，在轻微分散的云团中，可能从晕向星系和盘的内部迁移。
英文摘要：
Extreme scattering events in quasars suggest the existence of dark $\rm H_2 $ clumps of mass $\rm \sim 10^{-3} M_\odot$ and size $\rm \sim 10 AU$. Such clumps are extremely dense compared to WIMPs clumps of the same mass obtained by N-body simulations. A WIMP clump gravitationally attracted by a central $\rm H_2 $ clump would experience a first infall during which its density increases by $\rm 10^6$ in $\rm \sim 1 Myr$. In this poster I begin to explore the phenomenology of mixed clumps made with $\rm H_2 $ and WIMPs. Molecular clouds built with clumps are efficient machines to transform smooth distributions of WIMPs into concentrated networks. If WIMPs are neutralinos gravitationally attracted in clumps of such molecular clouds, they may either enrich the baryon sector over cosmological ages, or remain mixed with cold $\rm H_2 $ clouds until the clumps evaporate either by collision or by stellar UV heating. A phenomenological model based on an hypothetic dark baryonic component (DBC) that was invoked in the past to explain one of the main drawbacks of CDM profiles, their overly dense cores, is briefly revisited in this context. The DBC is replaced by a mix of $\rm H_2 $ and WIMPs, with a small fraction of HI produced by internal $\rm H_2 $ collisions, in slightly dispersive clumpy clouds that may migrate from the halo towards inner parts of a galaxy and disk.
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