Study Of The Infrared Solar Observation Techniques

The 1 M infrared solar telescope is the most important ground-based solar observational equipment in our country in the next fifteen years. All works in this dissertation are involved in the solar observational techniques and methods in the infrared, which is related with the above instrument. 1. For the telescope experiment platform, the solar spectrograph of Yunnan Observatory, the computer model of the spectral flux is established and is proven to be reliable. The spectral flux of FeJ 1 .56~im infrared solar spectrum is calculated by the model. The feasibility of the infrared observation on the current experiment platform and the reform methods are analyzed. 2. For the detector experiment platform, the PtSi infrared focal plane array camera, the model of the observational signal-to-noise ratio of FeI 1.56~tm lines is set up. Utilizing the model, how the varied noises influences the infrared observation is simulated. Based on these results, the infrared solar array observation of FeI 1 .56~tm lines is carried out successfully for the first time. 3. Under the current high-background and low-contrast observational circumstance, the image-processing techniques of the infrared solar spectrum are given, and the reasons and solving methods of the interference fringes appeared in observation are discussed in detail. ii 4. Utilizing the PVA material, the new generation near-infrared Stokes Polarimeter is designed and manufactured at 1 .S6prn. By use of the polarimeter mounted on the vertical spectrograph of the 2m McMath telescope at Kitt Peak, the two-dimensional Stokes I, Q, U, V parameters of a sunspot were observed. A set of new method to deduce vector magnetic field from Stokes parameters for FeI 1 .56~Arn zeeman-sensitive lines is put forward, and the deduced results from our infrared polarimeter are compared with those from Huairou Solar Magnetic Field Telescope. 5. For the solar spectrograph system of lm infrared solar telescope, the optical and mechanical designs of the vertical multi-wavelength bands spectrograph and the infrared large dispersion spectrograph are shown. 6. For the scientific objects of lm infrared solar telescope, the detector system of the vertical multi-wavelength bands spectrograph is designed, and the infrared detector system design used in the infrared large dispersion spectrograph is suggested also.