外掩类地行星日冕：模拟和敏感性
Externally Occulted Terrestrial Planet Finder Coronagraph: Simulations and Sensitivities
摘要：
天文学界正在积极采用多种日冕照相技术，用于对太阳系外类地行星进行天基直接探测和定性。典型的日冕仪有内部形状的焦平面和/或光瞳面掩模，可以阻挡和/或遮蔽星光，从而增加行星相对于母星的对比度。过去的研究表明，任何内部技术都受到感知和控制振幅、相位（波前）和偏振到精确水平的能力的限制-这就需要强调光学要求。另一种有前途的技术是在望远镜前方一定距离处放置一个遮光罩，即外部遮蔽器。这个遮光罩在进入望远镜之前抑制了大部分的星光-放松了对更传统望远镜的光学要求。虽然这是一个古老的技术，但最近由于认识到圆对称渐变切趾器可以很好地近似于成形的二元掩模而得到了发展。事实上，最佳的形状已经被设计成可以实现比传统日冕仪更小的内部工作角，并且还具有高的有效吞吐量，允许较小孔径望远镜实现与较大孔径望远镜相同的日冕仪分辨率和类似的灵敏度。在这里，我们报告我们正在进行的建模，模拟和优化的外部掩星，并显示灵敏度的结果相对于花瓣，光谱通带，菲涅尔传播的准确性和数量和形状的错误，并显示结果填充和分段孔径望远镜和讨论收购和传感的掩星的位置相对于望远镜。
英文摘要：
A multitude of coronagraphic techniques for the space-based direct detection and characterization of exo-solar terrestrial planets are actively being pursued by the astronomical community. Typical coronagraphs have internal shaped focal plane and/or pupil plane occulting masks which block and/or diffract starlight thereby increasing the planet's contrast with respect to its parent star. Past studies have shown that any internal technique is limited by the ability to sense and control amplitude, phase (wavefront) and polarization to exquisite levels - necessitating stressing optical requirements. An alternative and promising technique is to place a starshade, i.e. external occulter, at some distance in front of the telescope. This starshade suppresses most of the starlight before entering the telescope - relaxing optical requirements to that of a more conventional telescope. While an old technique it has been recently been advanced by the recognition that circularly symmetric graded apodizers can be well approximated by shaped binary occulting masks. Indeed optimal shapes have been designed that can achieve smaller inner working angles than conventional coronagraphs and yet have high effective throughput allowing smaller aperture telescopes to achieve the same coronagraphic resolution and similar sensitivity as larger ones. Herein we report on our ongoing modeling, simulation and optimization of external occulters and show sensitivity results with respect to number and shape errors of petals, spectral passband, accuracy of Fresnel propagation, and show results for both filled and segmented aperture telescopes and discuss acquisition and sensing of the occulter's location relative to the telescope.
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