二苯碳酰二肼柠檬酸盐光度法快速测定水中铬(Ⅵ)

合成了一种二苯碳酰二肼柠檬酸盐,建立了基于这种试剂和手持式光度计的铬(Ⅵ)的快速现场测定方法.在弱酸性介质中,此试剂与铬(Ⅵ)形成紫红色产物,λ_max=540nm,摩尔吸光系数ε=3.32×10⁴L·mol^-1·cm^-1,铬(Ⅵ)含量在0.03～2.00mg/L内符合比尔定律.该法用于电镀废水中铬(Ⅵ)的快速测定,结果令人满意.     

基于发光二极管探测器的太阳光度计的研究

介绍了一种采用商用发光二极管作为探测器的新型太阳光度计。阐述了系统的结构以及该仪器在监测气溶胶光学厚度领域的应用,并与传统的太阳光度计进行了对比试验。试验表明,两种仪器具有很好的一致性。     

Banach空间的K—M逼近

设Ｘ是自反、严格凸且具有Ｈ性质的Ｂａｎａｃｈ空间，Ａ是Ｘ的弱序列完备子集。本文证明了Ａ是可逼近紧的Ｃｈｅｂｙｓｈｅｖ集的充分必要条件是Ａ是太阳集；同时，也讨论了Ｏｒｌｉｃｚ序列空间的太阳集。     

孙子定理教学新探

改进了孙子定理的教学方法.     

The spectral observation of decimetric spikes with very high spectral resolution

Thousands of decimetric spikes were observed with a new spectrometer of Yunnan Observatory on June 24, 2001. The statistical analyses of the bandwidth, polarization degree, and half power duration of these spikes were made. We found that the absolute bandwidth of the spikes is down to the low limit of the instrument's spectral resolution (about 1.4 MHz). 76% of the total spikes have the polarization degree greater than 70%. The distribution of the half power durations concentrates on less than 16 milliseconds. These results support the interpretation of the electron cyclotron maser (ECM) mechanism for the decimetric spikes.     

多角度偏振成像仪遥感图像太阳耀斑区的拖尾校正方法

为了有效校正星载偏振相机成像时太阳耀斑区产生的拖尾,以高分五号卫星多角度偏振成像仪为例,结合多角度偏振成像仪在轨成像特点,理论分析了图像获取过程中拖尾产生的机理.建立了光斑区不含饱和像元情况下能够有效对漏光拖尾进行校正的矩阵法与暗行法校正模型,以及光斑区全像元饱和情况下结合矩阵法与暗行法估计光斑区饱和像元强度的遗留拖尾校正模型,该算法充分考虑了强光饱和条件下太阳耀斑区产生的漏光拖尾与遗留拖尾.利用实验室积分球光源成像光斑模拟在轨运行时遥感图像太阳耀斑开展拖尾校正方法可行性验证实验.实验结果表明,该方法不仅能有效去除图像中的拖尾噪声,提高图像质量,而且能够对光斑饱和像元强度进行有效估计.最后,分析多角度偏振成像仪在轨成像图中耀斑区拖尾对其辐亮度测量精度的影响,分析结果表明,拖尾校正前后,灰度方差由202.69×10^6下降至2.32×10^6,平均梯度由5.08×10^-1下降至2.26×10^-1.     

The study on fine structures in solar prominences

There are some solar prominence fine structures which are not observable. Thus, we need to use theoretical methods to study their geometric and physical properties. It is believed that observed intensities, and their fluctuations are related to such fine structures in the line of sight. Regarding the fact that analysis of intensity and its fluctuations necessitates the knowledge of the dependence of scattering albedo relative to optical depth, the present study is an attempt to determine scattering Albedo functions which are more probable to reality from the astrophysics’ perspective.     

Study of the size-flux relation of pores and spots

Using the vector magnetic field data from the Huairou Solar Observing Station of National Astronomical Observatories, a statistical study on the size-flux relation of photospheric magnetic features without any assumption is given. The selected data here include mature sunspots, as well as protosunspot (with a partial penumbra) and pore. We studied not only their size-flux relations of pore, protosunspot and mature sunspot, but also that of umbra and penumbra of the mature sunspots. The size-flux relationship of mature sunspots and their umbra and penumbra is found to be in different indexes of power-law. No evident relations are found between size and flux of the pores and protosunspots. We found that there is a threshold of 1×1012 Wb or (3-4.03) × 107 km2 for the transition from a pore to a protospot. Such results may be useful for understanding the physical conditions and dynamical processes of magnetic flux tubes in solar plasma during sunspot's formation. In addition, their characteristic size is also given.