Planetary microlensing at high magnification
Planetary microlensing at high magnification
复制标题
高倍率行星微透镜
DOI：
10.1046/j.1365-8711.2002.05607.x
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发表时间：
2002
影响因子：
4.8
通讯作者：
P. Yock
中科院分区：
文献类型：
--
作者：
N. Rattenbury;I. Bond;I. Bond;J. Skuljan;P. Yock
介绍了在集群计算机上进行的高倍率行星微透镜的模拟。研究发现，三分之二的行星引起的扰动发生在微透镜光曲线峰值的时间间隔[-0.5t F w H M, 0.5t F w H M]，其中t F w H M通常为~ 14小时。这意味着只有光曲线的这一部分需要对行星进行密集监测——这是一个非常重要的实际优势。在高倍率事件中，几乎所有的行星探测都不会涉及苛性交叉。我们讨论了在高倍率事件中确定行星参数所涉及的问题。如果地球质量的行星的轨道半径在1.5-2.5 au以内，那么用1m级的望远镜就可以探测到它们。在更大的区域可以探测到巨行星。对于多行星系统，单个行星引起的扰动在一定条件下是可以分离的。源恒星的大小需要独立确定，但源恒星上黑子的存在可能是可以忽略不计的，就像事件期间行星运动的影响一样。
Simulations of planetary microlensing at high magnification that were carried out on a cluster computer are presented. It was found that the perturbations owing to two-thirds of all planets occur in the time interval [-0.5t F w H M , 0.5t F W H M ] with respect to the peak of the microlensing light curve, where t F W H M is typically ∼ 14 h. This implies that only this restricted portion of the light curve need be intensively monitored for planets - a very significant practical advantage. Nearly all planetary detections in high-magnification events will not involve caustic crossings. We discuss the issues involved in determining the planetary parameters in high magnification events. Earth-mass planets may be detected with 1-m class telescopes if their projected orbital radii lie within about 1.5-2.5 au. Giant planets are detectable over a much larger region. For multiplanet systems the perturbations caused by individual planets can be separated under certain conditions. The size of the source star needs to be determined independently, but the presence of spots on the source star is likely to be negligible, as is the effect of planetary motion during an event.