A New Pupil for Detecting Extrasolar Planets
A New Pupil for Detecting Extrasolar Planets
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探测系外行星的新学生
DOI：
10.1117/12.856927
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发表时间：
2001
期刊：
影响因子：
--
通讯作者：
D. Spergel
中科院分区：
文献类型：
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作者：
D. Spergel
类地行星光学探测面临的挑战是行星与其主恒星之间 25 星等的亮度对比。本文介绍了一种新的光瞳设计，可沿其对称轴产生非常暗的零点。通过改变瞳孔的形状，我们可以控制这个零点的深度和位置。通过将该光瞳与屋顶消光器或猫眼消光器以及孔径光阑相结合，可以进一步增强该消光。光学系统的性能将受到镜面缺陷的限制。如果恒星在使用或不使用调零器的情况下成像，那么我们可以表征这些缺陷，然后用可变形镜纠正它们。当部署在 6 $\times$ 10 m 太空望远镜上时，完整的光学系统能够在 20 秒差距内探测到恒星周围的类地行星。对于围绕附近恒星（10 秒差距）的类地行星，望远镜可以通过测量 0.3 - 1.3 微米范围内的谱线来表征其大气层。
The challenge for optical detection of terrestial planet is the 25 magnitude brightness contrast between the planet and its host star. This paper introduces a new pupil design that produces a very dark null along its symmetry axis. By changing the shape of the pupil, we can control the depth and location of this null. This null can be further enhanced by combining this pupil with a rooftop nuller or cateye nuller and an aperture stop. The performance of the optical system will be limited by imperfections in the mirror surface. If the star is imaged with and without the nuller, then we can characterize these imperfections and then correct them with a deformable mirror. The full optical system when deployed on a 6 $\times$ 10 m space telescope is capable of detecting Earthlike planets around stars within 20 parsecs. For an Earthlike planet around a nearby stars (10 parsecs), the telescope can characterize its atmosphere by measuring spectral lines in the 0.3 - 1.3 micron range.