The Dark photon as an ultralight dark matter candidate can interact with the standard model particles via kinetic mixing. We propose to search for the ultralight dark photon dark matter using radio telescopes with solar observations. The dark photon dark matter can efficiently convert into photons in the outermost region of the solar atmosphere, the solar corona, where the plasma mass of photons is close to the dark photon rest mass. Because of the strong resonant conversion and benefiting from the short distance between the Sun and the Earth, the radio telescopes can lead the dark photon search sensitivity in the mass range of $4\times {10}^{-8}–4\times {10}^{-6}\mathrm{eV}$, corresponding to the frequency 10–1000 MHz. As a promising example, the low-frequency array telescope can reach the kinetic mixing $\epsilon \sim {10}^{-13}$ (${10}^{-14}$) within 1 (100) h of solar observations. The future experiment square kilometer array phase 1 can reach $\epsilon \sim {10}^{-16}–{10}^{-14}$ with 1 h of solar observations.

中文翻译：

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跨太阳的射频暗光子暗物质

作为超轻暗物质候选者的暗光子可以通过动力学混合与标准模型粒子相互作用。我们建议使用带有太阳观测的射电望远镜搜索超轻暗光子暗物质。暗光子暗物质可以在太阳大气的最外部区域，即日冕中有效地转化为光子，在该区域中，光子的等离子体质量接近于暗光子静止质量。由于强烈的共振转换，并且得益于太阳与地球之间的短距离，射电望远镜可以在质量范围内导致暗光子搜索灵敏度的提高。$4\times {10}^{-8}–4\times {10}^{-6}\mathrm{电子伏特}$，对应于10–1000 MHz的频率。作为一个有前途的例子，低频阵列望远镜可以达到动态混合$\epsilon 〜{10}^{-13}$ （${10}^{-14}$）在太阳观测的1（100）小时之内。未来的实验平方公里阵列第一阶段可以达到$\epsilon 〜{10}^{-16}–{10}^{-14}$ 1小时的太阳观测。