星系盘的垂直结构：非局域引力与暗物质的对比
The vertical structure of galactic discs: nonlocal gravity versus dark matter
AI总结：
本研究通过高分辨率N体模拟与解析推导，对比了非局域引力理论与标准暗物质模型下星系盘的垂直弯曲不稳定性，发现二者不稳定区域存在差异，为区分两种引力理论提供了新依据。
摘要：
近期的孤立星系模拟显示，修正引力理论下的星系盘形态与标准暗物质模型下的存在差异。本研究聚焦星系盘的垂直结构，对比了两种理论框架下星系盘在垂直方向的弯曲不稳定性。为此，我们利用高分辨率N体模拟，分别基于特定非局域引力理论（NLG）和标准暗物质模型构建了两个模型，并对比了它们抵御弯曲扰动的稳定性。我们的数值结果表明，NLG模型下星系盘的外缘区域更易出现不稳定性，而嵌入暗物质晕的星系盘则在中心区域更不稳定。随后我们基于弯曲波的色散关系对这些结果进行了解释，为此开展了解析研究以推导NLG下的色散关系，数值结果与解析模型的预测相符。由此我们得出结论：对星系盘弯曲不稳定性的分析可以解释两种理论下模拟星系盘所呈现的不同垂直结构。这些发现为区分修正引力模型与暗物质模型迈出了重要一步。
英文摘要：
Recent isolated galactic simulations show that the morphology of galactic discs in modified gravity differs from that of the standard dark matter model. In this study, we focused on the vertical structure of galactic discs and compared the bending instability in the vertical direction for both paradigms. To achieve this, we utilized high-resolution N-body simulations to construct two models in a specific nonlocal gravity theory (NLG) and the standard dark matter model and compared their stability against the bending perturbations. Our numerical results demonstrate that the outer regions of the disc are more susceptible to the instability in NLG, whereas the disc embedded in the dark matter halo is more unstable in the central regions. We then interpret these results based on the dispersion relation of the bending waves. To do so, we presented an analytical study to derive the dispersion relation in NLG. Our numerical results align with the predictions of our analytical models. Consequently, we conclude that the analysis of bending instability in galactic discs offers an explanation for the distinct vertical structures observed in simulated galactic discs under these two theories. These findings represent a significant step towards distinguishing between the modified gravity and dark matter models.
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