直接探测白矮星中的原子暗物质
Direct Detection of Atomic Dark Matter in White Dwarfs
摘要：
暗物质可能具有原子暗物质（aDM）形式的耗散非对称子成分。这出现在许多黑暗复杂性的场景中，并且是中性自然性的预测，例如镜像双希格斯模型。我们第一次展示了白矮星冷却如何在aDM上提供强大的约束。在暗光子和SM光子之间存在一个小的动力学混合的情况下，恒星预计会在其核心积累原子暗物质，然后以暗光子的形式辐射能量。在白矮星的情况下，这种能量损失可以对它们的冷却速度产生可检测的影响。我们使用测量的白矮星光度函数，严格约束的动力学混合参数之间的黑暗和可见光的光子，在DM质量的许多数量级，下降到值的$ε\sim 10^{-12}$。使用这种方法，我们可以限制的情况下，aDM构成的分数小$10^{-3}$的总暗物质密度。我们的方法与其他探测aDM的方法具有高度互补性，特别是在aDM被布置在黑暗磁盘中的情况下，这可能会使直接检测变得非常困难，但实际上会略微增强我们的冷却约束。
英文摘要：
Dark matter could have a dissipative asymmetric subcomponent in the form of atomic dark matter (aDM). This arises in many scenarios of dark complexity, and is a prediction of neutral naturalness, such as the Mirror Twin Higgs model. We show for the first time how White Dwarf cooling provides strong bounds on aDM. In the presence of a small kinetic mixing between the dark and SM photon, stars are expected to accumulate atomic dark matter in their cores, which then radiates away energy in the form of dark photons. In the case of white dwarfs, this energy loss can have a detectable impact on their cooling rate. We use measurements of the white dwarf luminosity function to tightly constrain the kinetic mixing parameter between the dark and visible photons, across many orders of magnitude in DM mass, down to values of $ε\sim 10^{-12}$. Using this method we can constrain scenarios in which aDM constitutes fractions as small as $10^{-3}$ of the total dark matter density. Our methods are highly complementary to other methods of probing aDM, especially in scenarios where the aDM is arranged in a dark disk, which can make direct detection extremely difficult but actually slightly enhances our cooling constraints.
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