对舰面温度数据的建模及其趋势和周期性分析

在系统建模理论的基础上,运用改进的动态数据建模方法,文章对某舰面温度数据进行建模并验证了模型的适用性,然后根据建立的模型进行了趋势和周期性分析。根据模型的适用性检验发现,对所研究的温度数据而言,ARMA(6,5)模型是最合适的,且其具有一定的线性趋势,但周期性不很明显。所有的建模和分析过程均在MATLAB上实现。     

数列算术平均序列的收敛性

对一般数列的情况进行了讨论,给出了数列的子列权的概念,得出了关于数列的算术平均序列的一个定理,即存在有限划分的收敛子列的数列,其算数平均序列收敛于其子列极限的线性组合,而系数正是相应子列的权。对其他的一些情况也进行了讨论。     

A new method of single celestial-body sun positioning based on theory of mechanisms

Considering defects of current single celestial-body positioning methods such as discon-tinuity and long period, a new sun positioning algorithm is herein put forward. Instead of tradi-tional astronomical spherical trigonometry and celestial coordinate system, the proposed new positioning algorithm is built by theory of mechanisms. Based on previously derived solar vector equations (from a C1R2P2 series mechanism), a further global positioning method is developed by inverse kinematics. The longitude and latitude coordinates expressed by Greenwich mean time (GMT) and solar vector in local coordinate system are formulated. Meanwhile, elimination method of multiple solutions, errors of longitude and latitude calculation are given. In addition, this algo-rithm has been integrated successfully into a mobile phone application to visualize sun positioning process. Results of theoretical verification and smart phone’s test demonstrate the validity of pre-sented coordinate’s expressions. Precision is shown as equivalent to current works and is acceptable to civil aviation requirement. This new method solves long-period problem in sun sight running fix-ing and improves applicability of sun positioning. Its methodology can inspire development of new sun positioning device. It would be more applicable to be combined with inertial navigation systems for overcoming discontinuity of celestial navigation systems and accumulative errors of inertial nav-igation systems.     

迎角／滚转角组合风洞试验中侧向弹性角的影响及处理方法

通过迎角／滚转角组合改变模型姿态是横向测力风洞试验中重要的试验方式,此类试验中虽然会提供侧向弹性角数据,但在使用试验数据时往往不使用侧向弹性角数据,这会使得气动载荷与模型姿态对应关系不准确。侧向弹性角由侧向力和偏航力矩引起,在侧向力和偏航力矩较大的试验中,侧向弹性角的影响尤为显著,如方向舵效率试验。本文通过分析侧向弹性角的影响,提出一种侧向弹性角数据处理方法,经试验应用表明可以有效地提高数据使用的准确性。     

喷注壁面外掠平板层流边界层速度和温度的HPM-Padé解析解

运用HPM-Padé(同伦摄动-帕德逼近)法导出了当喷注流体速度与距平板前缘距离的平方根成反比时,不可压缩常物性流体外掠平板层流边界层内无量纲速度和无量纲温度解析表达式,无量纲流函数1阶导数的HPM-Padé解析解与4阶龙格库塔法的数值解结果一致.利用HPM-Padé解析解研究了喷注系数和流体Prandtl数对速度和温度分布的影响.结果表明:Prandtl数越大,温度边界层越薄,壁面温度梯度越大;喷注系数越大,速度边界层厚度和温度边界层厚度越大,壁面速度梯度和壁面温度梯度越小,壁面喷注对平板有隔热作用;当喷注系数为0.619时,壁面的速度梯度和温度梯度为零,高温来流向壁面的传热被喷注流体完全阻隔.     

微牛级射频离子推力器结构优化研究

为了满足中国科学院空间引力波探测——"空间太极计划"对航天器推进系统提出的微牛量级推力高精度控制需求,基于感性耦合等离子体自持放电,设计了一套微牛级射频离子推力器(μRIT-1).通过理论分析与实验验证,完成了μRIT-1关键结构组件优化工作,包括射频天线、放电室及离子光学系统.根据实验结果,μRIT-1采用7匝线直径...     

自动编码器在流场降阶中的应用

自动编码器作为一种压缩算法,在数据降维和去噪等方面有着广泛实践,有条件作为一种降阶方法在流场识别与数据处理方面得到应用。文章中以圆柱绕流为例,首先对圆柱后速度场建立了编码模型,用来对原始数据进行降维和特征提取,之后将编码后的数据与流场特征量相关联,建立了由流场编码回归圆柱表面压力系数的神经网络,探索了降维后数据的应用。结果表明,自动编码得到的结果能够承载原始速度场的主要信息,解码后速度场与原速度场测试均方根误差小于0.02,压力回归测试均方根误差可小于0.1。说明自动编码器能够作为一种流场的特征提取和降阶方法,在未来得到更广泛的应用。     

Determination of Sulfur Abundance in the Solar Wind

Solar chemical abundances are determined by comparing solar photospheric spectra with synthetic ones obtained for different sets of abundances and physical conditions. Although such inferred results are reliable, they are model dependent. Therefore, one compares them with the values for the local interstellar medium (LISM). The argument is that they must be similar, but even for LISM abundance determinations models play a fundamental role (i.e., temperature fluctuations, clumpiness, photon leaks). There are still two possible comparisons—one with the meteoritic values and the second with solar wind abundances. In this work we derive a first estimation of the solar wind element ratios of sulfur relative to calcium and magnesium, two neighboring low-FIP elements, using 10 years of CELIAS/MTOF data. We compare the sulfur abundance with the abundance determined from spectroscopic observations and from solar energetic particles. Sulfur is a moderately volatile element, hence, meteoritic sulfur may be depleted relative to non-volatile elements, if compared to its original solar system value.     

跨声速半球柱绕流流场的激波系结构

本文在1相似文献   

SOHO contribution to the understanding of mass supply and flows in the solar corona

We expect a variety of dynamic phenomena in the quiescent non-flaring corona. Plasma flows, such as siphon flows or convective flows of chromospheric material evaporating into the corona, are expected whenever a pressure differences is established either between the footpoints or between the coronal and chromospheric segments of a coronal loop. Such flows can induce phenomena of spatial and temporal brightness variability of the corona. In particular, evaporation induces a net mass input into the corona and consequently coronal density enhancements. Flows are also expected in the regions where energy is released during magnetic reconnection. From the observational point of view the dynamics of the solar atmosphere has been investigated in great detail mostly in the lower transition region with the HRTS, and during flares with theSolar Maximum Mission andYohkoh. The high spectral, temporal and spatial resolution of theSOHO ultraviolet spectrometers should enable us in the near future to fill the gap providing a continuous coverage from the chromosphere to the corona, in the 10⁴–10⁶ K domain, and therefore to best study the dynamics throughout the solar atmosphere.