Vol 19, No 11 (2019) / Chen

The Lyman-alpha Solar Telescope (LST) for the ASO-S mission – II. design of LST

Bo Chen, Hui Li, Ke-Fei Song, Quan-Feng Guo, Pei-Jie Zhang, Ling-Ping He, Shuang Dai, Xiao-Dong Wang, Hai-Feng Wang, Chun-Long Liu, Hong-Ji Zhang, Guang Zhang, Yunqi Wang, Shi-Jie Liu, Hong-Xin Zhang, Lei Liu, Shi-Lei Mao, Yang Liu, Jia-Hao Peng, Peng Wang, Liang Sun, Zhen-Wei Han, Yan-Long Wang, Kun Wu, Guang-Xing Ding, Peng Zhou, Xin Zheng, Ming-Yi Xia, Qing-Wen Wu, Jin-Jiang Xie, Ya Chen, Shu-Mei Song, Hong Wang, Bo Zhu, Chang-Bo Chu, Wen-Gang Yang, Li Feng, Yu Huang, Wei-Qun Gan, Ying Li, Jing-Wei Li, Lei Lu, Jian-Chao Xue, Bei-Li Ying, Ming-Zhe Sun, Cheng Zhu, Wei-Min Bao, Lei Deng, Zeng-Shan Yin

Abstract

As one of the three payloads for the Advanced Space-based Solar Observatory (ASO-S) mission, the Lyman-alpha (Lyα) Solar Telescope (LST) is composed of three instruments: a Solar Corona Imager (SCI), a Lyα Solar Disk Imager (SDI) and a full-disk White-light Solar Telescope (WST). When working in-orbit, LST will simultaneously perform high-resolution imaging observations of all regions from the solar disk to the inner corona up to 2.5 R (R stands for the mean solar radius) with a spatial resolution of 4.8′′ and 1.2′′ for coronal and disk observations, respectively, and a temporal resolution of 30 – 120 s and 1 – 120 s for coronal and disk observations, respectively. The maximum exposure time can be up to 20 s due to precise pointing and image stabilization function. Among the three telescopes of LST, SCI is a dual-waveband coronagraph simultaneously and independently observing the inner corona in the HI Lyα (121.6±10 nm) line and white light (WL) (700±40 nm) wavebands by using a narrowband Lyα beam splitter and has a field of view (FOV) from 1.1 to 2.5 R. The stray-light suppression level can attain <10 −6 B (B is the brightness of the Sun) at 1.1 R and ≤5×10−8B at 2.5 R. SDI and WST are solar disk imagers working in the Lyα line and 360.0 nm wavebands, respectively, which adopt an off-axis two-mirror reflective structure with an FOV up to 1.2 R, covering the inner coronal edge area and relating to coronal imaging. We present the up-to-date design for the LST payload.

Keywords


telescopes — instrumentation: high angular resolution — Sun: flares — Sun: coronal mass ejections (CMEs) — Sun: UV radiation

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DOI: https://doi.org/10.1088/1674–4527/19/11/159

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