The Hollywood Strategy for Microlensing Detection of Planets
The Hollywood Strategy for Microlensing Detection of Planets
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好莱坞微透镜探测行星策略
DOI：
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发表时间：
1996
期刊：
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通讯作者：
A. Gould
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文献类型：
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作者：
A. Gould
跟着大明星走！我回顾了行星系统的检测和参数测量的理论，通过对正在进行的微透镜事件的后续观测。两个参数一般可以从事件本身测量：行星/星星质量比，$q$，和行星/星星分离的爱因斯坦环的单位。我强调监测事件的优势与巨星源更亮（因此更容易监测）和更大（从而提供了前景的测量有限源效应的额外参数：自行$\mu$）。在$q$和$\mu$之间存在潜在的强简并。我提出了一个简单的分析表示这种简并。然后，我描述了如何使用来自世界各地的天文台的精确的单波段测光，或来自单个站点的光学/红外测光，或最好两者兼而有之来打破它。这两种类型的观察正在进行或即将进行。对朝向核球的巨星事件的监测也是确定银河系内部的内容和结构的最佳方法。
Follow the big stars! I review the theory of detection and parameter measurement of planetary systems by follow-up observations of ongoing microlensing events. Two parameters can generically be measured from the event itself: the planet/star mass ratio, $q$, and the planet/star separation in units of the Einstein ring. I emphasize the advantages of monitoring events with giant-star sources which are brighter (thus easier to monitor) and bigger (thus offering the prospect of measuring an additional parameter from finite-source effects: the proper motion $\mu$). There is potentially a strong degeneracy between $q$ and $\mu$. I present a simple analytic representation of this degeneracy. I then describe how it can be broken using accurate single-band photometry from observatories around the world, or optical/infrared photometry from a single site, or preferably both. Both types of observations are underway or will be soon. Monitoring of giant-star events seen toward the bulge is also the best way to determine the content and structure of the inner Galaxy.