计算机打印口用作天文仪器接口

目前基本上所有天文仪器都是数字化的 ,几乎所有天文设备与计算机都有接口问题。我们在多套系统中采用计算机打印口来控制天文终端 ,认为这样做有不少好处。本文介绍了利用打印机接口天文仪器控制的技术 ,并给出两个例子     

Simulation Research on the Solar Hard X-Ray Imaging Telescope

The hard X-ray imaging telescope of the modulation collimator type is widely used in current solar observations. The spatial modulation telescope is the telescope which keeps its central axis not rotate, suitable for the satellite of 3-axis attitude stabilization. For the possible Chinese solar mission in the near future, we make a design of hard X-ray imaging telescope, and simulate the photon counting using the common simulation software GEANT4. Then we implement the image reconstruction with MATLAB, and compare the reconstructed image of the photons simulated by GEANT4 with that of the photons calculated by the geometric algorithm. The results show that the simulated one by GEANT4 is more closer to the reality than that obtained by the geometric algorithm. An executable design is also proposed at last.     

太阳活动极大和极小期太阳磁场周期变化研究

利用Wilcox天文台1975年到2010年间的太阳磁场数据,分析了太阳平均磁场在太阳活动极大和极小时期的短时周期性.结果显示太阳磁场主要具有9 d、13.5 d、27 d左右的周期.在太阳活动极大时期,27 d左右周期最为显著,而在太阳活动极小时期最显著的周期为13.5 d左右(1984～1986年间的太阳活动极小时期除外).这些结果说明太阳的活动区域在活动极大和极小时期具有明显不同的分布.     

利用台站资料定标太阳光度计效果评估

运用Langley方法、采用法国CE318太阳光度计在台站的观测记录为光度计定标,提出一种较客观的数据处理方法,主要分为4步：①利用Langley法对全年资料进行预处理,得到各通道定标常数、Langley法线性拟合相关系数、550nm的气溶胶光学厚度等;②以线性拟合相关系数的阈值大小（如440nm相关系数大于等于0．99）、定标期间550nm的平均气溶胶光学厚度小于等于0．15、半天（上午或下午）参与拟合的数据个数大于等于8组为条件,对预处理数据进行筛选;③根据光度计电压信号图像、最大值再次选取定标常数;④对最终选出的多组定标常数取平均值。对2002、2005年,乌鲁木齐、塔中、哈密、和田4个站点光度计资料进行试验,定标系数与出厂定标值（2002年）、北京定标值（2005年）比较后,4个站点的定标误差基本控制在8．5％以内（和田除外）,说明这种定标步骤有一定的参考价值。     

午后极光强度与行星际磁场的相关

利用1997年和199年南极中山站多通道扫描光度计的地面观测数据和WIND卫星在弓激波上游对行星际磁场(IMF)的观测数据,对午后高纬极光强度与IMF各分量、以及时钟角之间的相关进行了定量研究. 统计表明,630nm的强度Ir随IMF Bx的增大而减小,其线性相关系数为-0.3;而557.7nm的变化趋势与此相反,其相关系数要低得多. 630nm的强度随IMF By的变化曲线为一"V"形结构,其谷底在By=-3nT附近;557.7nm的强度也有相似的变化趋势,其谷底的位置在By=-2nT附近. 极光强度随IMF Bz的变化曲线为一倒着的"Z"字形结构. 630nm的强度随IMF的模B的增大而增强,其线性相关系数达到0.9,而557.7nm与B之间的相关性要差得多. 极光强度随IMF时钟角的变化曲线为一倒"V"结构,其反转点在θ=130°附近.     

A study on the asymmetries in flare lines

We calculate the H and CaII K profiles under different velocity models with chromospheric condensations and investigate the effect of the velocity in different layers on the profiles from a semi-empirical standpoint. The results show that the short-time, H blue asymmetry in the early stage of the flare can be caused by condensations in the transition zone, that the subsequent red asymmetry is the result of the downward motion of matter in the upper chromosphere, while the later CaII K asymmetries can be explained by downward velocities of 10–20 km/s in the middle and lower chromosphere.     

对地球质心偏移及板块驱动力的讨论

支持宇宙力参与板块运动的观点,赞同地球质心偏移的论断,但对质心偏移的力源和成因提出不同的看法。数理推导表明,太阳斥力与万有引力常数G的变化综合作用、冰盖在一极的形成与消融等是质心偏移的主要力源。     

Measurement of atmospheric total ozone by the filter photometric method

The total ozone content in the atmosphere was determined from the multichannel photometer observations of direct solar radiation made in the urban environment at Pune (18° 32 N, 73° 51E, 559 m ASL) and Sinhagad hill station (18° 22N, 73° 45E, 1305 m ASL) during March 1980-February 1982. The total ozone content of the atmosphere was computed making use of the differential absorption of solar radiation due to ozone at 0.4 and 0.6 m wavelengths in the Chappuis band. The values of the ozone data obtained from the photometer observations at Pune and Sinhagad were compared with the corresponding ozone data obtained from the Dobson spectrophotometer located at Pune. Values of ozone obtained by the photometric method were found to be smaller by 8–18% than the Dobson values when Vigroux's absorption coefficients were used. Similarly, when the absorption coefficients of Inn and Tanaka (1953) were used, the ozone values obtained by the photometric method were smaller by 4–14% than the Dobson values. The ozone values at the hill station obtained from the photometric method were in better agreement (5%) with the Dobson values.     

Supergene Geochemistry of Gold and Oxidation Zone of the Sain Us Gold Deposit in the Inner Mongolian Arid Region

The Sain Us gold deposit is a typical auriferous sulphide quartz vein deposit in the InnerMongolian arid steppe climatic region. The oxidation zone has been controlled by the arid cli-mate since the beginning of the Holocene. Gold supergene evolution is characterized by enlarge-ment of gold grains, complication of the gold form, raising of the gold grade and increase of thegold fineness; besides, gold and silver have two enrichment peaks at the same depth, which is insharp contrast to the unimodal enrichment of gold and silver and the occurrence of gold aboveand silver below in a humid climatic region. Sun pumping is the main cause for the bimodalenrichment of gold and silver. Illite 2 M_1 is one of the main causes for the upper enrichment peakof gold and silver.     

太阳辐射压摄动计算的新进展

介绍了一种新的建立太阳辐射压摄动模型的方法,即Ｖｏｋｒｏｕｈｌｉｃｋｙ等人提出的方法。该方法以辐射转移方程为基本数学工具,并运用相应的物理概念,通过对太阳辐射场强和辐射流量的计算来求出太阳辐射压摄动。此方法既适用于卫星处于地球半影区内和地球阴影之外的情形,也适用于地球反照辐射压的计算。还介绍了该方法的一些计算结果,并简单评述了其不足之处。