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暗能量的直接探测：XENON1T过剩和未来前景

Direct detection of dark energy: the XENON1T excess and future prospects

Sunny Vagnozzi, Luca Visinelli, Philippe Brax, Anne-Christine Davis, Jeremy Sakstein

备注：
24 pages, 5 figures. v3: included discussions on screening and propagation of dark energy quanta, added Table summarizing how screening is evaded in other stellar objects. Version accepted for publication in PRD. Cartoon version of our main results available in the source files. Code publicly available at https://github.com/lucavisinelli/XENONCHAM
发表信息：
Phys. Rev. D 104, 063023 (2021)
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摘要：

我们探讨了当前和即将到来的地面暗物质直接探测实验直接探测暗能量的前景。如果暗能量是由一个新的光自由度耦合到物质和光子驱动的，那么暗能量量子预计将在太阳中产生。这些量子自由地流向地球，在那里它们可以与标准模型粒子在直接探测实验的探测室中相互作用，这表明这些实验可以用来测试暗能量。屏蔽机制抑制了与新的轻粒子相关的第五种力，是许多暗能量模型的必要特征，它阻止了太阳核心的产生过程，同样，也阻止了红巨星、水平支星和白矮星核心的产生过程。相反，暗能量与光子的耦合导致了太阳速跃层的强磁场的产生，其机制类似于普里马科夫过程。这就允许在地球上探测到信号，同时避开了通常由新的轻粒子的恒星探测器产生的强烈约束。作为一个例子，我们研究是否可以通过变色龙屏蔽的暗能量来解释最近报道的XENON 1 T合作的电子反冲过剩，并发现这样一个模型是首选的背景只假设在$2.0σ$水平，在大范围的参数空间不排除恒星（或其他）探针。这增加了一种诱人的可能性，即XENON 1 T可能已经实现了对暗能量的首次直接探测。最后，我们研究了使用计划中的未来探测器（如XENONNT，PandaX-4 T和LUX-ZEPLIN）确认这种情况的前景。

英文摘要：

We explore the prospects for direct detection of dark energy by current and upcoming terrestrial dark matter direct detection experiments. If dark energy is driven by a new light degree of freedom coupled to matter and photons then dark energy quanta are predicted to be produced in the Sun. These quanta free-stream towards Earth where they can interact with Standard Model particles in the detection chambers of direct detection experiments, presenting the possibility that these experiments could be used to test dark energy. Screening mechanisms, which suppress fifth forces associated with new light particles, and are a necessary feature of many dark energy models, prevent production processes from occurring in the core of the Sun, and similarly, in the cores of red giant, horizontal branch, and white dwarf stars. Instead, the coupling of dark energy to photons leads to production in the strong magnetic field of the solar tachocline via a mechanism analogous to the Primakoff process. This then allows for detectable signals on Earth while evading the strong constraints that would typically result from stellar probes of new light particles. As an example, we examine whether the electron recoil excess recently reported by the XENON1T collaboration can be explained by chameleon-screened dark energy, and find that such a model is preferred over the background-only hypothesis at the $2.0σ$ level, in a large range of parameter space not excluded by stellar (or other) probes. This raises the tantalizing possibility that XENON1T may have achieved the first direct detection of dark energy. Finally, we study the prospects for confirming this scenario using planned future detectors such as XENONnT, PandaX-4T, and LUX-ZEPLIN.

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