光纤阵列太阳光学望远镜研究组知识库

太阳物理研究亟待解决的重大核心问题包括了太阳爆发、日冕加热和太阳风加速等机制.揭示这些现象背后的发生和发展规律将为空间灾害性天气预报和相关天体物理研究提供精确有效的模型.建议设计的日冕磁场和等离子体综合探测望远镜（COronal Magnetism and Plasma ASsembled Scopes,COMPASS）由口径为1.26 m大型日冕磁场探测望远镜（COronal Magnetism Probing Telescope,COMPT）、口径为0.30 m中型二维成像光谱日冕仪（Two-dimensional Spectroscopic Diagnosis Coronagraph,TSDC）以及安装在COMPT上的0.09 m的口径小型Lyot日冕仪（COMPASS-SC）组成.COMPT主攻高度范围0.05–0.65太阳半径(R_Sun)内矢量磁场和热动力学参量精确测量,TSDC聚焦在（0.10–1.50）R_Sun高度范围内对日冕等离子体的各项物理参量进行诊断以及提供全方位日冕结构和演化监测,而COMPASS-SC为COMPT提供其积分视场观测区域定位以及大视场日冕演化监测.这一组3台日冕仪功能互补互联,集中测量（0.05–1.50）R_Sun高度范围的矢量磁场和热动力学参量分布及其演化.由于其创新性设计,COMPT建成后不仅将成为国际上最大口径的折射式望远镜,也将成为第一台具有高偏振测量精度的多条谱线同时偏振成谱成像的日冕仪,而TSDC首次将白光偏振成像和谱线二维（线偏振）成像光谱测量功能集于一身.本文首先概括了COMPASS的科学需求和国外仪器的发展态势,然后从总体设计思想和理念、光机电初步设计等方面对COMPASS进行介绍,并特别阐述了围绕科学目标而做出的创新性仪器设计. 

Finding out and identifying mechanisms responsible for coronal eruptions, coronal heating and solar wind acceleration form the cores in solar physics research, and such mechanisms are crucial for us to establish efficient models for predicting the catastrophic space weather and even for sun-like stars. As one important element of the Ground-based Advanced Solar Observatory (ASO-G), the proposed COronal Magnetism and Plasma ASsembled Scopes (COMPASS) consist of three coronagraphs of different sizes. They are respectively the coronal magnetism probing refractive Lyot coronagraph with an aperture of 1.26 m, called COMPT, improved from American COSMO-LC, a two-dimensional spectroscopic diagnosis coronagraph with an aperture of 0.30 m, named TSDC, and a small Lyot coronagraph with an aperture of 0.09 m attached to COMPT for monitoring. Observations of COMPT focus on the accurate measurement of vector magnetic fields and other physical parameters in a height range of 0.0–0.65 solar radius above solar limb by two observing modes, the integral field Stokes spectroscopy (IFS) realized by a pair of integral field units and corresponding
spectrometers as well as two-dimensional imaging Stokes spectroscopy (TDIS) by dual tunable Lyot filters, and the reduced polarimetric optical switching is applied for high precision polarimetry, while observations from TSDC will provide information on the necessary physical parameters of coronal plasma in a field of view with height range from 0.10 to 1.5 solar radii, with help of Fabry-Perot interferometer to carry out the imaging spectroscopy as well as white light polarization imaging. These three coronagraphs form a complementary set. The scientific and observational goals are stated and then the preliminary optical, mechanical and electronic control designs of these coronagraphs are described. Finally the innovative ideas to serve the goals are outlined.