On ultraviolet freeze-in dark matter during reheating
On ultraviolet freeze-in dark matter during reheating
复制标题
再加热过程中紫外线冻结暗物质
DOI：
10.1088/1475-7516/2018/05/036
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发表时间：
2018
影响因子：
6.4
通讯作者：
Kang Zhaofeng
中科院分区：
文献类型：
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作者：
Chen Shao Long;Kang Zhaofeng
广泛的 DM 搜索没有任何确认信号，这促使我们超越传统的 WIMP 场景。弱相互作用大质量粒子 (FIMP) 范式提供了一个很好的替代方案，尽管它与热粒子的相互作用微弱，但仍然可以在没有传统 DM 信号的情况下正确产生遗迹丰度。基于可重整化算子的红外-FIMP通常存在非常小的耦合缺点，而基于高维有效算子的紫外-FIMP场景可以克服这一缺点。然而，它对早期宇宙的历史很敏感。先前的工作在再加热温度 TRH 处终止了这种敏感性。受其紫外线敏感性的推动，我们研究了更早的宇宙再加热时代的影响。我们发现，在TRH≫ mDM的通常情况下，只要有效算子维数d≤8，再加热期间的生产率就非常小。此外，我们考虑了在再加热期间可能产生的介体的贡献。此外，我们还研究了当TRH甚至低于mDM时的情况，如果DM的质量不超过TMAX，则可以在再加热过程中直接产生DM。
The absence of any confirmative signals from extensive DM searching motivates us to go beyond the conventional WIMPs scenario. The feebly interacting massive particles (FIMPs) paradigm provides a good alternative which, despite of its feebly interaction with the thermal particles, still could correctly produce relic abundance without conventional DM signals. The Infrared-FIMP based on the renormalizable operators is usually suffering the very tiny coupling drawback, which can be overcome in the UltraViolet-FIMP scenario based on high dimensional effective operators. However, it is sensitive to the history of the very early Universe. The previous works terminates this sensitivity at the reheating temperature TRH. We, motivated by its UV-sensitivity, investigate the effects from the even earlier Universe, reheating era. We find that in the usual case with TRH≫ mDM, the production rate during reheating is very small as long as the effective operators dimension d ⩽ 8. Besides, we consider the contribution from the mediator, which may be produced during reheating. Moreover, we study the situation when TRH is even lower than mDM and DM can be directly produced during reheating if its mass does not exceed TMAX.