Lobo-Parsaei-Riazi幽灵虫洞的银河引力微透镜：Paczyński光变曲线与概率特征
Galactic microlensing by Lobo-Parsaei-Riazi phantom wormhole: Paczyński light curves and probabilistic features
AI总结：
该研究推导LPR幽灵虫洞的弱场偏转角等微透镜物理量，计算其光变曲线等观测特征，并与史瓦西黑洞对比，为区分大质量与零质量幽灵虫洞提供观测依据。
AI中文摘要：
引力微透镜可提供区分大质量与零质量幽灵虫洞特征的潜在观测方法。本研究考虑受引力束缚的Lobo-Parsaei-Riazi幽灵虫洞（LPR）对银河的微透镜效应，假设源星位于银河核球和大麦哲伦云（LMC）中。我们推导了至四阶后牛顿近似的弱场偏转角，计算了爱因斯坦半径、爱因斯坦半径穿越时间及理想化点源的Paczyński型光变曲线；还在简化模型中估算了光学深度与事件率，该模型假设虫洞透镜受银河引力束缚。LPR参数γ与径向状态方程参数满足ω=1/γ，它影响ADM质量、爱因斯坦半径及微透镜时标。在大质量幽灵分支-1<γ<0中，主导偏转角项与1/r成正比，所得点源光变曲线类似Paczyński型；零质量对比情况γ=1则有质的不同，因为主导1/r项消失，可能出现沟槽。我们将理想化观测预测与史瓦西黑洞的对应预测进行了比较。
英文摘要：
Gravitational microlensing can provide a possible observational method for distinguishing between the signatures of massive and massless phantom wormholes. In this work, we consider Galactic microlensing by the bounded Lobo-Parsaei-Riazi phantom wormhole (LPR), assuming source stars located in the Galactic Bulge and in the Large Magellanic Cloud (LMC). We derive the weak-field deflection angle up to fourth post-Newtonian order and compute the Einstein radius, Einstein-radius crossing time, and idealized point-source Paczyński-type light curves. We also estimate the optical depth and event rate in a simplified model in which the wormhole lenses are assumed to be gravitationally bound to the Galaxy. The LPR parameter $γ$, which is related to the radial equation-of-state parameter by $ω= 1/ γ$, affects the ADM mass, the Einstein radius, and the microlensing timescale. In the massive phantom branch $-1 < γ< 0$, the leading deflection term is proportional to $1/r$, and the resulting point-source light curves are Paczyński-like. The massless comparison case $γ= 1$ is qualitatively different because the leading $1/r$ term vanishes and gutters may appear. The idealized observational predictions are compared with those for a Schwarzschild black hole.
