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

作者：Bo Chen, Hui Li, Kefei Song, Quanfeng Guo, Pei-Jie Zhang, Lingping He, Shuang Dai, Xiaodong Wang, Haifeng Wang, Chunlong Liu, Hongji Zhang, Guang Chun Zhang, Yunqi Wang, Shijie Liu, Hong-Xin Zhang, Lei Liu, Shilei Mao, Yang Liu, Jia-Hao Peng, Peng Wang, Liang Sun, Yang Liu, Zhenwei Han, Yanlong Wang, Kun Wu, Guang-Xing Ding, Peng Zhou, Xin Zheng, Ming-Yi Xia, Qingwen Wu, Jin-Jiang Xie, Ya Chen, Shumei Song, Hong Wang, Bo Zhu, Chang-Bo Chu, Wengang Yang, Li Ying Feng, Yu Huang, Wei-Qun Gan, Ying Li, Jingwei Li, Lei Lu, Jianchao Xue, Beili Ying, Mingzhe Sun, Cheng Zhu, Weimin Bao, Lei Deng, Zengshan Yin · 发表于：Research in Astronomy and Astrophysics · 年份：2019 · DOI：10.1088/1674-4527/19/11/159 · 被引用次数：45 · 研究领域：Solar and Space Plasma Dynamics、Stellar, planetary, and galactic studies、Astro and Planetary Science

Abstract As one of the three payloads for the Advanced Space-based Solar Observatory (ASO-S) mission, the Lyman-alpha (Ly α ) Solar Telescope (LST) is composed of three instruments: a Solar Corona Imager (SCI), a Ly α 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 Ly α (121.6±10 nm) line and white light (WL) (700±40 nm) wavebands by using a narrowband Ly α 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 mean brightness of the solar disk) at 1.1 R ⊙ and ≤5×10 −8 B ⊙ at 2.5 R ⊙ . SDI and WST are solar disk imagers working in the Ly α 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...