AI 中文总结
本文介绍引力微透镜行星探测方法，其可探测雪线外宽轨道行星，补充其他探测技术，还讨论从光变曲线提取天体参数及建模示例，助力行星形成研究。
AI 中文摘要
引力微透镜是一种独特的行星探测方法，不依赖于探测主星或行星的光线，而是通过行星的引力场扰动遥远光源发出的光线来发现行星。该方法的机制具有多项优势：它能够探测不同类型主星周围、系统雪线处及以外的各种质量的宽轨道行星，因此微透镜技术与其他更敏感于近轨道或大质量行星的探测技术形成互补。在本章中，我们回顾了微透镜方法，并讨论如何从微透镜光变曲线或额外的高角分辨率观测中提取质量、距离等物理属性。微透镜对于系外行星统计研究的更广泛背景至关重要，因为它可以对雪线以外宽轨道上的行星施加约束，研究这一参数空间有助于我们揭示行星形成的细节以及我们太阳系的形成过程。最后，我们提供了一个示例，说明如何对光变曲线进行建模并获取主星和行星的准确物理参数。
英文摘要
Gravitational microlensing is a unique planet-detection method that does not rely on detecting light from the host star or planet. Instead, planets are discovered when their gravitational field perturbs the light coming from a distant source. The mechanics of this method offer several advantages. It has the ability to detect wide-orbit planets of various masses around host stars of different types, at and beyond the system's snow line. Thus, microlensing complements the other detecting techniques that are more sensitive to close-orbit or high-mass planets. In this Chapter, we review the microlensing method and discuss how the physical properties, such as mass and distance, can be extracted from the microlensing light curve or from additional high-angular resolution observations. Microlensing is essential for the broader context of exoplanet demographics, as it can place constraints on planets, in wide orbits, beyond the {\it snow line}. Studying this parameter space can help us unravel the details of planet formation and how our own Solar System formed. Lastly, we provide an example of how to model a light curve and obtain accurate physical parameters for the host and planet.
CommentsThis work is a peer-reviewed chapter contribution to an edited volume
