改进的万有引力公式

根据广义相对论给出的行星运动方程，导出如下改进的万有引力公式F＝－GMm/r^2-3G^2M^2mp/c^2r^4应用该公式可给出光线近日偏折问题的准确解。     

Thermospheric neutral density response to solar forcing

Recent measurements by the Solar EUV (Extreme Ultra Violet) Experiment (SEE) aboard the Thermosphere–Ionosphere–Mesosphere Energetics and Dynamics satellite (TIMED) provide solar EUV spectral irradiance with adequate spectral and temporal resolution, and thus the opportunity to use solar measurements directly in upper atmospheric general circulation models. Thermospheric neutral density is simulated with the NCAR Thermosphere–Ionosphere–Electrodynamic General Circulation Model (TIEGCM) using TIMED/SEE measurements and using the EUVAC solar proxy model. Neutral density is also calculated using the NRLMSISE-00 empirical model. These modeled densities are then compared to density measurements derived from satellite drag data. It is found that using measured solar irradiance in the general circulation model can improve density calculations compared to using the solar proxy model. It is also found that the general circulation model can improve upon the empirical model in simulating geomagnetic storm effects and the solar cycle variation of neutral density.     

广义Lefschetz数的粘接公式的应用

本文通过研究拓扑空间上幂等自映射在基本群上诱导的作用和点同伦，得到与之同伦的，具有较好性质的自映射。并利用自映射这些性质，使用广义Lefschetz数的粘接公式，得到幂等自映射的Nielsen数不超过1的结论。     

Frictional resistance of supercritical pressure RP-3 flowing in a vertically downward tube at constant heat fluxes

Based on the demands of compact heat exchangers and micro cooling channels applied for aviation thermal protection, the flow resistance characteristics of aviation kerosene RP-3 were experimentally studied in a vertically downward circular miniature tube with an inner diameter of 1.86 mm at supercritical pressures and constant heat fluxes. A long and short tube method was used to accurately calculate the frictional pressure drop, and experimental conditions are supercritical pressures of 4 MPa, mass flow rates of 2–4 g/s (i.e., mass fluxes of 736–1472 kg/(m²?s)), heat fluxes of 100–500 kW/m², and inlet temperatures of 373–673 K. Results show that the sharp variations of thermophysical properties, especially density, have significant influences on frictional resistances. Generally, the frictional pressure drop and the friction factor increase with increasing inlet temperatures, and this trend speeds up in the relatively high-temperature region. However, the friction factor has a sudden decline when the fuel outlet temperature exceeds the pseudo-critical temperature. The frictional pressure drop and the friction factor basically remain unchanged with increasing heat flux when the inlet temperature is relatively low, but increase quickly when the inlet temperature is relatively high. Besides, a larger mass flux yields a higher pressure drop but does not necessarily yield a higher friction factor. Finally, an empirical friction factor correlation is proposed and shows better predictive performance than those of previous models.     

基于EMD的无参考图像清晰度评价方法

针对现有的灰度变化统计函数不能提供图像全频段综合评价的缺陷,提出了一种新的基于经验模式分解的无参考清晰度评价方法。图像经经验模式分解后,会产生多层本征模式函数图像和剩余图像。不同本征模式函数图像包含了不同频率区间的边缘、纹理信息。模糊图像和清晰图像在相同本征模式函数分解层上,表现出不同的灰度变化特性。通过统计各层本征模式函数图像的极值个数,作等权重加和,并利用整幅图像像素数进行归一化处理,构建了经验模式分解清晰度参数。仿真模糊图像和遥感图像的试验结果验证了该参数评价清晰度的有效性。     

随机振动试验谱形参数计算方法

介绍采用解析方法计算随机振动试验参考谱形的主要参数，给出了计算谱值参数和总均方根值的计算公式和具体计算实例。     

对《离散数学》中三个公式、定义及定理的研究

本文对《离散数学》中三个公式、定义及定理进行了充分的研究及透彻的分析，分别给出了这三个公式、定义及定理的简化形式及其规律，使得它们变的浅显易懂。而这些无论对老师还是对学生都是十分重要的。     

线性系统采样Z变换的一个递推公式

本文给出了计算1/(s a)~n的采样z变换的递推公式,证明了其分子多项式系数的对称性质,外对α为复数的情况进行了推广。     

An empirical model for the variation of rain drop size distribution with rain rate at a few locations in southern India

A Joss–Waldvogel impact type disdrometer was installed at four different locations in the Indian peninsula during various periods from 2001 till date. The data are analysed to study the nature of rain drop size distribution (DSD) in this region. Out of the three well known distributions that describe DSD, namely, the Marshall–Palmer, Gamma and Lognormal, it has been found that Lognormal distribution fits the DSD in this region better than the other ones. Lognormal distributions for different rain rates were then derived by fitting the lognormal function to the data using a curve fitting software. Then the variation of fit parameters with rain rate was evaluated. Incorporating these variations, into the Lognormal distribution, an empirical equation that describes the DSD in this region for different rain rates was derived. Then this equation was tested with sample data from each of these stations. The data used for validation were not used for fitting lognormal equation to derive the fit parameters. The correlation between the DSD measured and derived using the empirical model was found to be quite good (0.9) except in some cases where the coefficient dropped to 0.75. The empirical model can be updated when more data are available.     

An empirical model of electron density in low latitude at 600 km obtained by Hinotori satellite

An empirical model of electron density (Ne) was constructed by using the data obtained with an impedance probe on board Japanese Hinotori satellite. The satellite was in circular orbit of the height of 600 km with the inclination of 31 degrees from February 1981 to June 1982. The constructed model gives Ne at any local time with the time resolution of 90 min and between −25 and 25 degrees in magnetic latitude with its resolution of 5 degrees in the range of F_10.7 from 150 to 250 under the condition of K_p < 4. Spline interpolations are applied to the functions of day of year, geomagnetic latitude and solar local time, and linear interpolation is applied to the function of F_10.7. Longitude dependence of Ne is not taken into account. Our density model can reproduce solar local time variation of electron density at 600 km altitude better than current International Reference Ionosphere (IRI2001) model which overestimates Ne in night time and underestimates Ne in day time. Our density model together with electron temperature model which has been constructed before will enable more understanding of upper ionospheric phenomenon in the equatorial region.