摘要
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 LyαSolar 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 to20 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 Lyαbeam 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 Lyαline 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.
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 to20 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.
基金
supported by Chinese Academy of Sciences (CAS)
supported by the National Natural Science Foundation of China (Grant Nos. 11427803, U1731241, U1731114 and U1531106)
the CAS Strategic Pioneer Program on Space Science (Grant Nos. XDA04076100, XDA15052200, XDA15320103 and XDA15320301)
