关于行星际磁场螺旋扇形过渡区稳定性的分析

本文利用四层模式,讨论了ME型行星际磁场螺旋扇形过渡区的稳定性。结果表明:(1)ME型过渡区中可以激发三种大尺度波动,且三种波动都存在低频截止;(2)随着波数k增大,不稳定性的增长率都有上升的趋势,但其中A型波动的增长率存在一个极大值和一个极小值;(3)当k与扇形区中太阳风速度V_q呈平行或反平行时,波动最易被激发;随着k与V_q之间夹角变大,截止波长逐渐向短波段移动;当k与V_q相垂直时,波动则不能被激发;(4)当k与V_q夹角呈75°时,可以激发波长为5×104km、相速为340 km/s的波动,这与Voyager 1飞船在磁层顶处的观测结果相一致。由此推断,螺旋扇形过渡区中激发的波动可能是导致磁层顶K-H不稳定性的一种扰动源。      

脉冲微分系统关于部分变元的强稳定性

介绍了一种新的稳定性——脉冲微分系统的解关于部分变元的强稳定性,并进而讨论了该类稳定性问题. 首先建立了两个重要的引理,然后再借助于逐段连续的Lyapunov函数,得到了脉冲微分系统的零解关于部分变元强稳定性的一些判定定理.最后阐述了这些定理的应用.      

行星际磁场的螺旋扇形过渡区

从行星际磁场的大尺度螺旋形构型和扇形边界附近太阳风流动与冕旒的可能相关,本文得到一个推论,即在行星际空间可能存在一种较厚的螺旋扇形过渡区。行星际磁场和太阳风的实地观测证实了这种较厚的螺旋扇形过渡区的存在。在所分析的45个螺旋扇形过渡区中,磁场强度都不为零;大部分大于或小于周围平均场强。本文进一步分析了磁增大和磁减小两类过渡区中的物理性质和可能成因。      

冕洞网络的大气模型

本文采用非径向磁流管位形的假设,计算了太阳冕洞网络部分的色球-日冕过渡区的能量平衡模型。所考虑的能量流包括辐射、传导、对流和机械波加热（如阿尔芬波）,计算结果表明在冕洞网络部分的过渡区中,电子温度T和密度N分别比宁静太阳中的值低60%和2倍,而其过渡区的厚度比宁静太阳中的大4倍。这种大气模型可满意地解释T≥105K范围的远紫外观测发射量度的分布。另外我们也发现在冕洞大气的过渡区中,阿尔芬波加热似乎不能忽略,尤其是在冕洞的过渡区底部,它的加热作用可能会超过热传导。在冕洞大气中,由于波动量的淀积而产生的对流能损耗也是重要的,在过渡区底部650km以上,对流能损耗逐渐超过辐射损耗。      

冲击波在变密度、运动介质中的传播

本文得到了点源爆炸波在变密度、运动介质中传播的分析解(ω=2,γ=5/3),讨论了耀斑引起的击波在太阳风中传播的一些特性。发现1AU附近区域恰是击波各种重要效应的过渡区;击波减速等效指数i(D=K(u_o,E_s)R-i(u_o,E_s,R))是介质运动速度u_o.击波能量E_s,和击波传播距离R的函数,通常是小于1/2的,不是自型理论预言的那样简单;太阳风的对流效应使击波可以传播到10-20AU以远,与飞船(先躯者10、11号)新近的观测相吻合。      

精细积分方法的稳定性和精度分析

分析了结构动力分析的精细积分方法的稳定性、精度和计算工作量,讨论了离散时间间隔、指数矩阵幂级数展开式的截断阶数L以及2N类算法的阶数N的优化问题.说明了精细积分方法是条件稳定的.综合考虑稳定性、精度和计算工作量,判定截断阶数L取4时精细积分方法的总体效果最好,并给出了N的参数优化公式.最后给出2个例题验证了稳定性和精度分析的正确性.     

用于电子测量仪器设计的Wien电桥理论研究

深入分析了用于电子测量仪器设计的Ｗｉｅｎ电桥振荡器及其变型Ｍｅａｃｈａｍ桥振荡器,给出了提高振幅与频率稳定性、减少波形失真的技术措施。讨论了电压控制式Ｗｉｅｎ电桥振荡器的构成。此外,讨论了Ｍｅａｃｈａｍ型晶体振荡器,给出的电路可作为真空计测量低层大气的压强（７６０￣１０－１Ｔｏｒｒ）。并可用于宇航测量中,以监中能的物理效应。     

机械臂的区间二型模糊超螺旋滑模控制

针对不确定性条件下机械臂的轨迹跟踪问题,提出一种基于区间二型模糊逼近扰动的超螺旋滑模控制方法.首先将机械臂的建模误差、摩擦项、外部扰动等均视为广义扰动,然后利用自适应区间二型模糊逼近广义扰动.接着通过一个嵌套自适应律来设计基于超螺旋算法的趋近律,进而提出超螺旋滑模控制器.通过Lyapunov稳定性理论验证了趋近律的稳定性,基于此证明了系统的稳定性,并导出了区间二型模糊自适应律.仿真实验表明,区间二型模糊具有更好的逼近效果,超螺旋滑模控制能够抑制系统的扰动,本文所提算法具有响应快速和鲁棒性强的优点.     

万有引力场中带挠性附件充液卫星的姿态稳定性

本文利用能量-Casimir方法讨论万有引力场中带挠性附件非对称全充液卫星的姿态稳定性, 导出此刚-弹-液系统在轨道坐标系内相对平衡的稳定性充分条件.      

农林飞机近地作业飞行的纵向稳定特性

分析了农林飞机近地作业飞行的纵向气动力特性,讨论了存在地面效应时的纵向静稳定性准则及主要气动导数对静稳定性的影响;根据地效区内飞机的五阶小扰动运动线化方程,计算了农林飞机近地作业飞行的模态特性,并运用特征矢量研究了各模态中起主要作用的运动变量;利用Routh判据对农林飞机近地作业飞行的纵向动稳定性进行了分析,通过简化推导了存在地面效应时保证飞机动稳定性其重心的位置要求.研究结果表明,农林飞机近地作业飞行时地面效应对其纵向气动特性及稳定性的影响不可忽略.      

Energy balance and stability

Recent theoretical work pertaining to the energy balance and stability of stellar coronae is reviewed. While in magnetically confined coronal regions coronal heating balances only the radiation losses of the corona and transition region, open regions can also lose energy by means of stellar wind and outward thermal conduction. The relative importance of these kinds of energy losses, and the asymptotic properties of the stellar wind, depend sensitively on the radial distribution of the energy input. Solar coronal models, both for open and closed regions, can often be applied to other stars. The requirements for which this is possible are briefly discussed. Stability analyses that are not restricted to the corona alone, but rather include the transition region and upper chromosphere, are important for our understanding of the detailed energy balance of outer stellar atmospheres. The stability of the complete system chromosphere/transition region/corona is probably closely related to the recent observational result that with increasing stellar activity the coronal radiation increases faster than the chromospheric radiation.     

基于Transition SST模型的高雷诺数圆柱绕流数值研究

为了研究高雷诺数下圆柱绕流边界层的转捩现象和圆柱尾迹近壁区的流动特征,首先通过在典型雷诺数下采用Transition SST四方程转捩模型模拟圆柱绕流得到的结果与实验结果及采用SST k-ω两方程湍流模型模拟结果的对比分析,验证了Transition SST模型在模拟高雷诺数下圆柱绕流的优越性,并较为准确地预测出了圆柱绕流边界层的转捩现象及尾迹近壁区的流动特征。然后分别对亚临界区、临界区、超临界区和过临界区的圆柱绕流问题进行了数值模拟,分析了不同雷诺数下圆柱绕流的流场结构及圆柱表面压力系数、摩擦力系数的变化规律,研究了圆柱绕流近壁区的流动特征、边界层转捩的流动机理、转捩位置及其随雷诺数的变化规律。结果表明,亚临界区二维圆柱绕流边界层发生层流分离,无分离泡和转捩现象;临界区和超临界区二维圆柱绕流边界层先产生了分离泡现象,之后流动发生了转捩并在转捩后发生湍流分离;过临界区二维圆柱绕流边界层流动在转捩之后发生湍流分离,无分离泡现象;在临界区、超临界区和过临界区,二维圆柱绕流边界层转捩位置随雷诺数增大向前驻点移动。     

Quality variation of GPS satellite clocks on-orbit using IGS clock products

Over 60% clocks on board of the GPS satellites are working longer than their designed life. Therefore realizing their stabilities in a long time scales is essential to GPS navigation and positioning plus IGS time scale maintaining. IGS clock products from 2001 to 2010 are used to analyze the GPS satellite clock qualities such as frequency stabilities and clock noise level. We find out that for the clocks of Block IIA satellites the frequency stabilities and clock noise are 10 times worse than that of the Block IIR and IIR-M satellites. Moreover, the linear relationships between frequency stabilities and clock residuals have been deduced with an accuracy of better than 0.02 ns. Specially, it is noticed that the clock of the PRN27 is instable and the relationship between the frequency stability and residuals is at least a quadratic curve. Therefore, we suggested that GPS satellite clocks should be weighted by their quality levels in application, and the observations of the Block IIA should not be used for real-time positioning which required precision better than one meter.     

Extreme ultraviolet observations of the solar corona: First results from the coronal diagnostic spectrometer on SOHO

We present first results from the Coronal Diagnostic Spectrometer (CDS) aboard the ESA/NASA Solar and Heliospheric Observatory (SOHO). CDS is a double spectrometer operating in the 151–785 Å range. This region of the solar spectrum is rich in emission lines from trace elements in the solar atmosphere, which can be used to derive diagnostic information on coronal and transition region plasmas. Early spectra are presented and well identified lines are listed. In addition, examples of images in selected wavelength ranges are shown, for a prominence, a loop system and a bright point, demonstrating well the power of such extreme ultraviolet observations.     

Model of a fluxtube with a twisted magnetic field in the stratified solar atmosphere

We build a single vertical straight magnetic fluxtube spanning the solar photosphere and the transition region which does not expand with height. We assume that the fluxtube containing twisted magnetic fields is in magnetohydrostatic equilibrium within a realistic stratified atmosphere subject to solar gravity. Incorporating specific forms of current density and gas pressure in the Grad–Shafranov equation, we solve the magnetic flux function, and find it to be separable with a Coulomb wave function in radial direction while the vertical part of the solution decreases exponentially. We employ improved fluxtube boundary conditions and take a realistic ambient external pressure for the photosphere to transition region, to derive a family of solutions for reasonable values of the fluxtube radius and magnetic field strength at the base of the axis that are the free parameters in our model. We find that our model estimates are consistent with the magnetic field strength and the radii of Magnetic bright points (MBPs) as estimated from observations. We also derive thermodynamic quantities inside the fluxtube.     

磁场强度对日冕定态结构的影响

以二维ＭＨＤ模型及时变方法为基础,内外边界完整的设影特征线边界条件,考察了太阳日冕大气的定态结构随偶极场强度的变化情况。模拟结果表明：随着偶极场强度的增加,磁场对太阳风的约束增强,低纬闭磁场打开程度减少,高纬与低纬区速度差增加,并且在阿尔文马赫数为１的点附近达到最大,速度过度区变陡;随着日心距离增加,低纬区宽度减小,速度过渡区变陡,可定性解释Ｕｌｙｓｓｅｓ飞船的新观测事实。     

聚碳酸酯微孔塑料的动态力学热分析

通过对聚碳酸酯微孔塑料进行动态力学热分析,得到了不同密度微孔塑料动态力学性能的温度图谱和频率图谱,研究了储能模量和损耗因子与温度、频率及密度之间的变化规律和玻璃化转变温度与密度之间的关系.结果表明:在高频或低温时,随着温度的升高,微孔塑料储能模量降低,损耗因子增加;当温度高于材料的玻璃化转变温度或者频率较低时,随着频率的降低和温度的升高,储能模量和损耗因子都急剧地降低;聚碳酸酯微孔塑料的玻璃化转变温度T_g在175°C左右,次级转变在70~100℃之间,结果与密度几乎无关.