Overview: The space gravitational wave detection telescope is one of the core payloads of the gravitational wave detection satellite, simultaneously expanding and contracting the transmitted beam. Optical path stability is one of the core indices for the telescope, closely related to its structural stability. To meet the ultra-high path stability and structural stability requirements posed by the gravitational wave detection mission, it is essential to study the structural deformation measurement of the telescope. Currently, there are still several shortcomings in the research of multi-degree-of-freedom deformation measurement methods for gravitational wave detection telescopes, such as inaccurate selection of measurement points, inability to decouple multi-degree-of-freedom coupling, and unclear identification of error sources in multi-degree-of-freedom measurement. This paper deeply investigates the high-precision measurement of structural deformation of space-borne telescopes designed for space gravitational wave detection. It preliminarily establishes a framework and method system for measuring the structural deformation of space-borne telescopes, theoretically describing the measurement principle of the method. The feasibility of this method applied to space gravitational wave detection is verified through simulation analysis and error decomposition. The paper focuses on resolving the issue of decoupling multiple degrees of freedom, establishing a mathematical model using analytical methods, and conducting preliminary validation using Zemax. Finally, noise analysis of the measurement system is carried out, with experimental testing of the main noise components in the measurement system, validating the correctness of the theoretical noise model proposed in this paper. The experimental results show that near 1 Hz, the displacement noise background of the single-link interferometer is 100 pm/Hz^1/2. At 1 mHz in the low-frequency range, the displacement noise background reaches 10 nm/Hz^1/2. The noise level of the measurement system below 1 mHz is mainly limited by environmental temperature noise, while above 10 mHz, it is primarily constrained by laser frequency noise, phase acquisition background noise, and vibration noise. During the development phase of the space gravitational wave detection telescope, the research on this measurement method is expected to fulfill the telescope's multi-degree-of-freedom deformation measurement needs. It also provides data feedback for telescope design and offers guidance for the study of the telescope's optical path stability.

混混响室复杂强电磁环境下开展材料屏蔽效能测试是电磁防护领域的研究热点。研究边界形变互耦混响室屏蔽效能测试系统性能，开展了动态范围、电场分布特性和不确定度三个方面的试验验证，结果表明：在实际测试中，测试结果小于60 dB即为可信测试值；在1～10 GHz频段内，互耦混响室发射室的空间电场标准偏差小于3 dB，接收室的空间电场标准偏差小于2 dB，满足国际、国内相关标准要求，场均匀性良好；测试系统的扩展不确定度为5.90 dB，可以作为材料屏蔽效能测试平台使用。

研制了基于三分区镜的倒立式三视场施密特型望远镜，对其关键技术进行了分析。利用正三棱锥的几何对称性，推导了3个视场的视轴夹角与分区镜面夹角之间的关系式，设计了用于实现多视场观测功能的三分区镜；通过有限元法分析了倒立式施密特望远镜主镜重力形变对像质的影响，阐述了检测光路关键参数对施密特修正镜加工误差的影响程度，采用蒙特卡罗法对该光学系统的杂散光进行了分析。最后对整个光学系统进行了实验检测，检测结果表明：实际研制的三分区镜镜面之间的夹角为133.08°，可同时对相互垂直的3个视场进行观测；该望远镜光学系统的PV=0.614λ，RMS = 0.105 λ(λ= 632.8 nm)。该系统可用于地球空间姿态测量，拓展了施密特望远镜的应用范围。

通过实验和仿真的方法，研究了多点分布的内部热源加热作用对紧凑型双路TEA CO₂激光器谐振腔热稳定性的影响。采用直流风扇热交换抑制了高压电源的局部加热效应，通过调整热交换的效率，可在13~22 ℃环境温度范围内，使前后谐振腔镜受到的局部加热形变作用和环境温度引起的热胀冷缩作用基本抵消。为实现更宽温度范围的谐振腔稳定性，在有效热交换措施的基础上，根据模拟预测的形变规律，提出了谐振腔变形的角度补偿方法。使用传感器获得环境温度与设定初始环境温度的偏差，通过调整伺服电机步数实现对方位角的补偿，补偿值约0.28 step/℃，通过PZT促动器调整悬臂调谐结构末端位移，实现对俯仰角的补偿，补偿值约0.79 μm/℃。