The Lyman-alpha Solar Telescope (LST) for the ASO-S mission - II. design of LST
The Lyman-alpha Solar Telescope (LST) for the ASO-S mission - II. design of LST
复制标题
用于 ASO-S 任务的莱曼阿尔法太阳望远镜 (LST) - II。
DOI：
10.1088/1674-4527/19/11/159
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发表时间：
2019
影响因子：
1.8
通讯作者：
Han Zhe
中科院分区：
文献类型：
--
作者：
Chen Bo;Li Hui;Song Ke-Fei;Guo Quan-Feng;Zhang Pei-Jie;He Ling-Ping;Dai Shuang;Wang Xiao-Dong;Wang Hai-Feng;Liu Chun-Long;Zhang Hong-Ji;Zhang Guang;Wang Yunqi;Liu Shi-Jie;Zhang Hong-Xin;Liu Lei;Mao Shi-Lei;Liu Yang;Peng Jia-Hao;Wang Peng;Sun Liang;Han Zhe
莱曼-阿尔法（Lyα）太阳望远镜（LST）是先进天基太阳天文台（ASO-S）任务的三个有效载荷之一，由太阳日冕成像仪（SCI）、Lyα太阳圆盘成像仪（SDI）和全盘白光太阳望远镜（WST）三部仪器组成。在轨道上工作时，LST将同时对太阳日冕至内日冕2.5 R⊙（R⊙代表太阳平均半径）以内的所有区域进行高分辨率成像观测，日冕和日冕观测的空间分辨率分别为4.8 “和1.2 ”，日冕和日冕观测的时间分辨率分别为30-120秒和1-120秒。由于精确的指向和图像稳定功能，最长曝光时间可达20秒。在LST的三台望远镜中，SCI是一台双波段日冕仪，利用窄带Lyα分束器在HI Lyα（121.6±10 nm）线和白光（700±40 nm）波段同时独立观测内日冕，视场（FOV）为1.1 ~ 2.5 R⊙。杂散光抑制水平在1.1 R⊙下可达到< 10−6 B⊙（B⊙为太阳盘的平均亮度），在2.5 R⊙下可达到≤5× 10−8 B⊙。SDI和WST是分别工作在Lyα线和360.0 nm波段的太阳盘成像仪，采用离轴双镜反射结构，视场可达1.2 R⊙，覆盖日冕内边缘区域，与日冕成像有关。我们提出了LST有效载荷的最新设计。
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 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 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.