AI 中文总结
该研究用三分量薛定谔-泊松模拟探究宇宙学矢量暗物质中的核晕关系，从矢量场初始条件出发，发现非线性演化及普罗卡星凝聚体，得出两者质量经验关系，还研究了物体矢量场结构，为相关未来研究提供重要输入。
AI 中文摘要
我们使用三分量薛定谔-泊松模拟研究了矢量暗物质中的宇宙学核晕关系。从宇宙学矢量场初始条件出发，由于暴胀期间矢量场的演化，小尺度上得到增强。我们发现，在物质-辐射相等后几乎立即开始非线性演化，并在晕中心产生致密的自引力普罗卡星凝聚体。通过径向密度分布确认中心凝聚体后，我们发现普罗卡星质量与晕质量之间的经验关系为\(\widetilde M_\star\propto \widetilde M_{\rm h}^{0.6403}\)，不过有趣的是，我们仅能在约10%的晕中确认普罗卡星。这为矢量暗物质模型中普罗卡星的丰度和合并率的未来研究提供了重要输入。我们还通过全局纵向和横向极化分数以及晕内局部自旋密度研究了这些物体的矢量场结构，其随宇宙时间增加。
英文摘要
We study the cosmological core-halo relation in vector dark matter using three-component Schrödinger-Poisson simulations. Starting from cosmological vector-field initial conditions, which due to the evolution of the vector field during inflation are enhanced on small scales, we find that nonlinear evolution begins almost immediately following matter-radiation equality and produces compact self-gravitating Proca-star condensates at the centers of halos. After confirming the central condensates through their radial density profiles, we find the empirical relation \(\widetilde M_\star\propto \widetilde M_{\rm h}^{0.6403}\) between the Proca star mass and halo mass, although interestingly we find that we are only able to confirm Proca stars in $\mathcal{O}(10\%)$ of halos. This serves as important input for future studies of the abundance and merger rates of Proca stars in models of vector dark matter. We also examine the vector-field structure of the objects through global longitudinal and transverse polarization fractions and local spin density inside halos, which increases over cosmic time.
Comments9 pages, 8 figures
