东台吉乃尔盐湖卤水比蒸发系数测定及回归方程

东台吉乃尔盐湖卤水属于Na+，K+，Mg(2+)／Cl，SO—H2O对五元水盐体系，体系比较复杂，卤水在蒸发过程中结晶的盐类繁杂，影响卤水蒸发率的离子较多，同时东台吉乃尔盐湖地处气候条件特殊的柴达木盆地腹地。本文配合开发东台吉乃尔盐湖卤水资源所采用的工艺要求，对不同阶段影响卤水蒸发速率的多种气象参数和卤水性质进行了比较详细的测定，并进一步建立了相应的回归标准方程。     

基于可靠性指标的Ratio检验模糊度质量方法

整周模糊度估值的可靠性对保障卫星导航定位精度有着至关重要作用,本文针对常规Ratio检验模糊度方法中阈值c难以确定问题,基于模糊度成功率检验理论分析了Ratio检验法的概率特性,推导了模糊度失败率与Ratio检验阈值间的函数关系式,实现利用给定可靠性指标——模糊度失败率确定Ratio检验阈值c,从而保证模糊度固定解的可靠性。算例表明,该方法可解决Ratio检验中阈值c动态取值的关键问题,具有一定的实际意义。     

基于ASTER VNIR SWIR多光谱遥感数据识别与提取干旱地区岩性信息——以西南天山柯坪隆起东部为例

ASTER多光谱遥感数据目前可以用于岩石矿物资源信息的识别和提取。本研究尝试利用ASTER 可见光近红外（VNIR）和短波红外（SWIR）的多光谱遥感数据提取干旱地区的岩石与矿物信息。基于新疆天山西南缘柯坪隆起东部不同地层单元岩石的化学组成和矿物成份以及VNIR SWIR谱域光谱吸收特征的分析,我们采用相关吸收波段深度（RBD）和波段比值（BR）方法对研究区的多光谱遥感数据进行图像处理,有效区分和识别了白云岩、石灰岩、砂岩以及阿克苏群的蓝片岩—绿片岩和砂质片岩。白云岩的CO2-3吸收谱带中心波长位于232〖KG*3〗μm,与灰岩的CO2-3 吸收谱带中心波长位置235 μm相比,具有向短波长方向移动的特点,据此可以利用RBD7、RBD8分别有效的识别白云岩和灰岩; 长英质岩石显示Al OH和Fe3+ VNIR SWIR吸收特征,而基性 超基性岩石显示Fe2+ 和Fe、Mg OH特征,利用不同的铁价态和次要矿物可以区分它们：ASTER band2/band1代表了含Fe3+ 矿物分布信息、ASTER band5/band4代表了含Fe2+ 矿物分布信息、RBD6可以估计Al OH矿物的丰度; 砂质/泥质片岩含较多的多硅白云母、绿泥石、黑硬绿泥石以及风化后表面覆盖的其它粘土矿物,在221 μm（band 6）存在有特征的吸收谱带,并且在165 μm（band 4）具有较高的反射率,而蓝片/绿片岩在221 μm（band 6）反射率较高,不具有明显特征吸收谱带,同时其在165 μm（band 4）反射率较低,因此蓝片/绿片岩ASTER band4/band6 比值低。应用ASTER band4/band6波段比值可以有效的区分开砂质/泥质片岩与蓝片岩/绿片岩。     

Experimental Study on Conversion Efficiency of A Floating OWC Pentagonal Backward Bent Duct Buoy Wave Energy Converter

Wave tank tests were carried out to evaluate the total efficiency of a floating OWC Pentagonal Backward Bent Duct Buoy (PBBDB). Two kinds of turbine generators were used in tests. The incident wave power, pneumatic power and electricity were measured. The test results show that the primary efficiency can reach up to 185.98% in regular waves and 85.86% in irregular waves. The total efficiency from wave to wire with Wells turbine-generator set is 33.43% in regular waves and 15.82% in irregular waves. The peak total efficiency of the PBBDB with check valves equipped with the impulse turbine-generator set is 41.68% in regular waves and 27.10% in irregular waves. The efficiency of the turbine-generator set is about 30% in the tests. Obviously, the total efficiency can be further improved with the increasing of turbine efficiency.     

The stability of the pristine magnetopause

A MHD theory of combined Kelvin-Helmholtz (KH) and Rayleigh-Taylor (RT) instabilities for a transition layer with two different scale lengths (Δ and δ for the variation of velocity/magnetic fields and density, respectively) is presented. The study is motivated by reports of magnetopauses with no low latitude boundary layer, in which a sharp density drop over a distance δ?Δ is observed (“pristine” magnetopauses (J. Geophys. Res. 101 (1996) 49). The theory ignores compressibility effects and applies to subsonic regions of the dayside magnetopause. The RT effect is included to account for temporary periods of acceleration of the magnetopause, caused by sudden changes of the solar wind dynamic pressure. For small wavelengths λ, such that δ?λ?Δ, a WKB solution shows that the velocity gradient operates, together with magnetic tensions, to attenuate or even stabilize the Rayleigh-Taylor instability within a certain wavelength range. An exact dispersion relation for flute modes, valid for all λ, in the form of a fourth order polynomial for the complex frequency ω, is obtained from a model with a constant velocity gradient, dV/dy within Δ, and with δ→0. Flute modes are possible because of the existence of bands of very small magnetic shear on the dayside magnetopause (J. Geophys. Res. 103 (1998) 6703). The exact solution allows for a study of the change of the action of the velocity gradient with λ from the long-λ range where dV/dy is KH destabilizing to the short-λ range where dV/dy produces a stabilizing effect. Both, the WKB approximation and the well known tangential discontinuity model (Δ→0) are recovered as limiting cases of the exact solution. Properties of the KH and RT instabilities, for different density ratios on either side of the magnetopause, are described. For flute modes, at very small λ the RT instability grows faster and becomes the dominant effect. However, it is shown that the growth rate remains bounded at a finite value as λ→0, when a theory with a finite δ model is considered. To study configurations with finite, arbitrary, δ/Δ ratios, the MHD perturbation equations are solved numerically, using hyperbolic tangent functions for both the density and velocity transitions across the magnetopause. To examine the influence of different δ/Δ ratios on the growth rates of KH and RT, calculations are performed for different δ/Δ, with and without acceleration, and for two different density ratios. It is found that the general features exhibited by the constant dV/dy model, are confirmed by these numerical solutions. The stability of pristine magnetopauses, and the possibility of observing some theoretical predictions during magnetopause crossings in ongoing missions, are discussed.     

The Relationships of Sunspot Magnetic Field Strength with Sunspot Area, Umbral Area and Penumbra-Umbra Radius Ratio

Stokes profile inversion is very important to get the information on the vector magnetic field. Because the magnetic fields cannot be directly observed, adopting Stokes spectrum analysis to obtain vector magnetic field has become the major technique recently. Therefore, by Stokes profile inversion, we obtained vector magnetic fields of two layers based on the numerical solution (DELO solution, ReEs et al., 1989) to the polarized radiative transfer equation. We analyze the relationships of sunspot magnetic field strength with sunspot area, umbral area and penumbra-umbra radius ratio. By statistical research, it is found that the field strengths of the upper layer and the lower one decrease with the increasing penumbra-umbra radius ratio, and that the logarithmic expression is able to fit well the relationship between the maximum field strength of the upper layer and the sunspot area. Furthermore, we verify the result obtained by Ringnes and Jensen (1961) about the relationship between the maximum magnetic field strength and the umbral area, and the result obtained by Antalová (1991) of the relationship between the field strength and the penumbra-umbra radius ratio.     

行星变速箱传动比方案的计算机辅助设计

传动比方案设计是行星变速箱ＣＡＤ技术中的关键问题之一。本文应用行星变速箱基本设计理论和计算机技术，建立了行星变速箱传动比方案ＣＡＤ软件，为有关科研部门及生产企业的产品开发提供了一种有效手段。     

砂泥岩地层地应力纵向分布特征与规律

以实际沉积地层中抽象出来的砂泥岩地层概念模型为研究对象, 在盆地构造力学、岩石力学性质分析的基础上, 采用应力场数值模拟法研究分析砂泥岩地层中的纵向地应力分布特征和规律。研究结果表明, 水平主应力在砂泥岩的分界面发生突变, 变化程度主要与两侧岩石的力学性质差异相关, 也与区域构造应力有一定关联; 杨氏模量对最大水平主应力影响程度大于对最小水平主应力的影响, 泊松比对地层最小水平主应力影响程度大于对最大水平主应力的影响。杨氏模量和泊松比对最大水平主应力的影响, 在伸展应力状态下前者影响相对较小, 走滑应力状态下, 影响程度基本相同, 挤压应力状态下, 前者影响程度相对较大; 而对于最小水平主应力的影响, 在三种应力状态下, 泊松比的影响均大于杨氏模量。地层的岩性变化方式(渐变或突变)对地层最小水平应力差产生显著影响, 厚度变化对地层最小水平应力差大小无影响。上述认识可以指导砂泥岩地层的压裂和储层改造, 改善压裂效果。     

土壤水分及土壤-大气界面对麦田水热传输的作用

文章根据1996年在中国栾城农业生态试验站观测的田间试验资料,分析了土壤水分和土壤-大气界面对麦田水热传输的抑制和加速作用。对于显热和潜热输送,土壤水分起决定作用,土壤水分越小,显热通量越大,潜热通量越小,反之亦然。只在土壤水分较小时界面厚度对显热和潜热输送作用较大。对于土壤热输送,界面厚度起决定作用,界面厚度越大土壤热通量越小。分析还发现60cm深处土壤水势与叶水势和大气水势的相关系数较其它深度处的土壤水势大。0～60cm土层是确定土壤水分运动对界面水热传输影响的一个良好的指示层。     

基于构造应力场资料的加卸载响应比方法研究

引入中国大陆构造应力场资料,结合区域构造及断层运动特征,根据岩石力学原理确定优质破裂面,对走滑断层、正断层和逆断层３种主要断层运动形式,推导了有效剪应力表达式;提出了新的加卸载判定,并对部分震例进行了再研究。