We study here a novel application of Kim and Lee charged wormholes assuming them to be dark halo objects playing the role of lenses in the Galactic microlensing with source stars belonging to the Galactic Bulge and the Large Magellanic Cloud. First, we observe that both the backreacted scalar (\(\alpha \)) and electrically (Q) charged wormholes have the same zero ADM mass as has the background Ellis–Bronnikov wormhole having a special equation of state parameter \(\gamma = - 1\). In particular, we argue that, for \(\alpha \ne 0\), the solution formally resembles, but can at best be sourcewise different from, that of the background wormhole. The charge (\(Q\ne 0\)) thus provides an extra degree of freedom that introduces a non-trivial redshift function \(\Phi \) to the background, alters its throat radius to \(r_{{\text {th}}}\), yet keeps the wormhole massless. Second, we focus on this electrically charged case and calculate the light deflection angle up to 4th PPN order, analyze the effect of Q on the lensing observables such as the image positions, magnification, centroid and time delay of images of the source stars. Third, we analyze the probabilistic features such as optical depth and event rate estimated on the basis of the hypothesis that the wormhole lens could be bound or unbound to our Galaxy. Finally, we report an intriguing qualitative prediction that, compared to the Schwarzschild black hole, the Paczyński light curves of the electrically charged wormhole are much dimmer that also show characteristic gutters at the times the source enters and exits the Einstein ring. The gutters gradually come together as Q approaches the extreme limit \(\frac{r_{{\text {th}}}}{\sqrt{2}}\), at which the Einstein radius \(R_{E}\) vanishes so that the source crosses it instantly. It is speculated that re-analyzing past data on Galactic microlensing may betray the presence of charged wormholes.

我们在这里研究金和李带电虫洞的新颖应用，假设它们是暗晕物体，在银河微透镜中扮演透镜的角色，源恒星属于银河核球和大麦哲伦星云。首先，我们观察到反反应标量（\(\alpha \)）和带电（Q）带电虫洞具有与背景埃利斯-布朗尼科夫虫洞相同的零ADM质量，具有特殊的状态参数方程\(\gamma = - 1\) .特别是，我们认为，对于\(\alpha \ne 0\)，解决方案在形式上类似于背景虫洞的解决方案，但最多可以在源方面有所不同。因此，电荷 ( \(Q\ne 0\) ) 提供了额外的自由度，将非平凡的红移函数\(\Phi \)引入背景，将其喉部半径更改为\(r_{{\text { th}}}\)，但保持虫洞无质量。其次，我们关注这种带电情况，计算高达 4 阶 PPN 阶的光偏转角，分析Q对源星图像的图像位置、放大倍数、质心和时间延迟等透镜观测量的影响。第三，我们分析了基于虫洞透镜可能与我们的银河系绑定或未绑定的假设估计的概率特征，例如光学深度和事件率。最后，我们报告了一个有趣的定性预测，即与史瓦西黑洞相比，带电虫洞的帕辛斯基光变曲线要暗得多，并且在光源进入和离开爱因斯坦环时也显示出特征性的沟槽。当Q接近极限\(\frac{r_{{\text {th}}}}{\sqrt{2}}\)时，沟槽逐渐聚集在一起，此时爱因斯坦半径\(R_{E}\)消失，因此源立即穿过它。据推测，重新分析过去有关银河微透镜的数据可能会暴露带电虫洞的存在。