计量仪器的平均值检验

通过实例介绍了平均值检验的原理、方法及其在生产实践中的应用。     

用定标块准确确定圆度仪的放大倍数

用定标块校准圆度仪的放大倍数时，一般是将定标块在圆度仪上测量的圆记录放大轮廓图用同心圆模板对线，找出凹下轮廓的径向放大值，然后除以定标块小平面弦高的实际值，其商即为放大倍数。但是，这种方法的缺点是测量准确度不高，不适用于圆度仪自动化程度日益提高带来的快速数字采样自动化校准放大倍数的要求。根据未抑制的定标块圆记录放大轮廓的凹下部分为一弦线的特点，推导了式（８）～（１３）。按要求的采样相邻点的夹角在弦线中点附近的直线上找出三个连续采样值，代入式（８）～（１３），可准确计算出圆度仪的放大倍数。用实例验证了这种新方法的准确性和可行性。     

误差分离法测圆柱度误差的不确定度估计

阐述五测头误差分离法在普通机床上实现圆柱度误差在位测量的原理和方法，并对测量不确定度进行了全面的分析和估计，明确了测量精度范围。此不确定度分析有助于机床误差的修正和补偿，对其它形状误差的精密测量和误差分离技术的实际应用具有普遍意义。     

万工显误差修正不确定度分析与计算

分析影响万工显测量精度的误差因素，以单项误差修正为基础，对仪器的多项误差进行全面修正，并对修正后的仪器测量不确定度进行分析与计算。     

形位误差在位测量的误差分离技术

采用误差分离原理，对大型工件的几何精度实施在位测量，可以将基准的误差从测量结果中分离出来，从而减少测量不确定度，提高测量精度。     

单次测量值的检验采用格拉布斯准则检验论证

根据国内实际情况，提出在微波功率计量质量保证方案中。对单次测量值的检验采用格拉布斯准则检验，并对它进行了论证。     

高频大功率GXN—50型霓虹灯电子电源的研制

ＧＸＮ－５０型霓虹灯电子电源是为负载提供高频交流电压电流的电源设备，是一种专用大功率霓虹灯电源。该产品采用先进的电子技术，节能效率高，带负载能力强（比传统电源高４倍以上），并采用超音技术，用特制的电子开关代替价格昂贵的机械继电器，因而无任何噪声，灯光变化采用程序控制，变换方式灵活，工作稳定可靠。该电源体积小、重量轻，并设计了过压过流保护电路，具有抗干扰能力强等特点。     

非正态分布误差的统计处理

列举常见的非正态分布误差，综述常见非正态误差的概率分布及其特征量，误差分布律的估计及检验，非正态误差的常用统计处理方法及其评定与合成。     

中低温光纤辐射测温技术的研究

以国产石英光纤作光路、硫化铅探测器为敏感元件所构成的中温光纤辐射测温仪，在２００℃以上实现了１℃分辨力的温度检测；以氟化物光纤作光路、硒化铅探测器为敏感元件，初步实验结果是８０℃以上获得了１℃的分辨力。提出一种新的桥路双平衡调解法，较好地解决了半导体探测器的温漂问题。系统所采用的积分与累加检测法对噪声与干扰有明显的抑制作用。     

光学非球面检测系统的精度仿真分析

在分析非球面检测仪的测量精度时，用一般的不确定度评定方法难于得到符合实际的结果。现采用计算机仿真分析的方法来分析其测量不确定度，以确保仪器研制的成功。结果表明，计算机仿真的确是一种既经济又高效的方法，在现代误差和精度理论中有重要的作用。     

热流效应对场向电流确定的影响

给出了任意速度分布函数条件下复频率的介电函数和色散关系的求解方法. 讨论了16矩近似条件下, 场向热流对电子速度分布函数, 介电函数实部与虚部, 以及离子与电子谐振频率和阻尼率的影响, 并与平衡态时麦克斯韦分布等离子体的计算结果进行了比较. 忽略场向热流效应, 正向电子漂移速度条件下, 上行等离子线探测, 会过高估计场向电流; 负向电子漂移速度条件下, 上行等离子线探测会过低估计场向电流. 对上下行等离子线同时探测情况, 忽略热流效应同样会过高估计场向电流.      

移动载体上天线工作角域分析

静止轨道卫星与地球上移动载体间的数据通信时,要求移动载体在运动中始终保持通信链路信号不中断。从移动载体看卫星的仰角和方位角随移动载体在地球上的位置及其自身的姿态(方位,俯仰,滚动)而变,因此要求载体上天线既具有极宽的辐射方向图特性和良好的圆极化特性。按静止轨道卫星定点位置、载体工作地域、载体运动中姿态角(方位角、俯仰角、滚动角)变化范围,导出移动载体上天线实际需要的工作角域,为载体上天线辐射特性的设计给出了依据。     

Method for the prediction of the effective dose equivalent to the crew of the International Space Station

This paper describes a methodology for assessing the pre-mission exposure of space crew aboard the International Space Station (ISS) in terms of an effective dose equivalent. In this approach, the PHITS Monte Carlo code was used to assess the particle transport of galactic cosmic radiation (GCR) and trapped radiation for solar maximum and minimum conditions through an aluminum shield thickness. From these predicted spectra, and using fluence-to-dose conversion factors, a scaling ratio of the effective dose equivalent rate to the ICRU ambient dose equivalent rate at a 10 mm depth was determined. Only contributions from secondary neutrons, protons, and alpha particles were considered in this analysis.     

Consequences of the application of the streamer fluid model to the study of the sprite inception mechanism

We present the results of a streamer-fluid model used to investigate the electrodynamical coupling between the troposphere and upper atmosphere due to the penetration of lightning electric fields into the mesosphere and the lower ionosphere, generating sprites. The model solves the continuity equation for electrons and ions coupled to Poisson equation. The dominant physical response of the atmosphere is the formation of a screening-ionization wave. The wave shields the atmosphere above it from the action of the lightning field and, together with the conductivity reduction below it due to attachment, the wave amplifies the total field below it, allowing for the penetration of intense electric fields in the mesosphere as it propagates downwards into regions of higher density that compress the wave. This is the key physical mechanism for sprite inception. We evaluated the effects of the thundercloud charge geometry, lightning current waveshape, atmospheric conductivity, via different electron density profiles, and the effect of ionization, attachment and electron mobility coefficients in the electrical breakdown process, related to halo production, and sprite streamer initiation. The results showed that electrons with higher mobility are more efficient in shielding the lightning electric field before breakdown, causing delay, and they contribute to the formation of the streamer seed after breakdown, anticipating the sprite streamer inception. Similarly, a higher effective ionization rate, produced by modifications in the attachment and ionization coefficients, anticipates sprite inception. The simulations with 6 different electron density profiles, and therefore conductivities, spanning 4 orders of magnitude, showed that the altitude of breakdown and sprite initiation, as well as their time delays from the lightning discharge are directly related to atmospheric conductivity: higher conductivities produce halo and sprite inception at lower altitudes with longer delays and may hinder sprite formation. We document that variations of 30 times in the lightning current leads to sprite initiation altitudes in the range 66.0–73.5 km, with delays between 1.550 and 34.500 ms, while variations of 4 orders of magnitude in the conductivity profile lead to initiation altitudes 61.0–70.6 km, with delays in the range 3.825–9.825 ms. Consequently, we suggest that lightning characteristics dominate over atmospheric parameters in determining sprites’ initiation altitude and delay. The simulation of a −CG, with a constant current of 30 kA, did not produce a sprite seed, confirming an asymmetry in the response of the atmosphere to positive and negative lightning. This is due to the free electron drift direction that is away from the screening ionization wave, preventing the formation of the streamer seed for the great majority of −CGs. The same does not apply to halos, which depend on the occurrence of breakdown and can be produced by discharges of both polarities.     

落塔微重力水平激光干涉测量方法中的干扰因素分析

落塔是获得微重力环境的重要设施,落塔微重力水平的测量对微重力科学实验的研究至关重要. 激光干涉是测量落塔微重力水平的一种新方法,这种方法的基本原理是让一个参考落体在落舱中自由下落,落舱由于受到服外空气阻力的作用将与自由落体运动略有差异,1 11. 肫内的参考落体则更接近理想的自由落体运动,这就使得落舱与参考落体之间存在着加速度差,这种加速度差便反映了落服的微重力水平,其所导致的相对运动则可通过激光干涉的方法测量出来. 本文对落塔微重力水平的激光干涉测量方法中将会遇到的一些主要干扰因素进行了分析,计算结果表明,这些干扰网素所造成的总误差约为 1.2 x 10-7g,低于微重力水平的预测值 10-4~lO-6 g,因此该方法是一种比较可行的测量方法.      

火星地形对火星大气运动的影响及火星尘暴发生的可能机制

本文在准地转模式的假定下,讨论了火星地形对火星大气的影响,并根据文章所提供的信息对火星尘暴发生的物理机制作了粗略的解释。      

辐射变色薄膜剂量计性能测试及加速器应用

本课题的目的是建立用于辐射加工高剂量水平吸收剂量测量的辐射变色薄膜剂量计。通过系统研究,批量制备了以尼龙为基材,副品红氰化物为染料的辐射变色薄膜剂量计。为了验证批制辐射变色薄膜剂量测量的可靠性,选择了国际上应用较广的FWT-60膜及丙氨酸薄膜剂量计与本实验室批制的辐射变色薄膜开展实验室内剂量比对,比对结果均在±4%内符合,归一化偏差En绝对值均小于1。通过在加速器上进一步应用实验表明批制辐射变色薄膜可用于电子束辐照参数测量。     

Animal models for the study of the effects of spaceflight on the immune system.

Animal models have been used to determine the effects of spaceflight on the immune system. Rats and rhesus monkeys have been the primary animals used for actual space flight studies, but mice have also been utilized for studies in ground-based models. The primary ground based model used has been hindlimb unloading of rodents, which is similar to the chronic bed-rest model for humans. A variety of immune responses have been shown to be modified when animals are hindlimb unloaded. These results parallel those observed when animals are flown in space. In general, immune responses are depressed in animals maintained in the hindlimb unloading model or flown in space. These results raise the possibility that spaceflight could result in decreased resistance to infection in animals.     

Intermittence of the short-term periodicities of the flare index

Intermittence of the short-term periodicities (25–35 days) of the flare index are investigated using the wavelet transform method for the full-disc and for the northern and the southern hemispheres of the Sun separately over the epoch since 1966 until 2002. The wavelet transform results show that occurence of periodicities of flare index power is highly intermittent in time. The period-averaged wavelet power of the flare index presents this fact very clearly displaying independence of flaring activity on the solar hemispheres in several time intervals over almost four solar cycles under study. Moreover correlations of the period-averaged wavelet power of the flare index for the separate hemispheres and for the full-disc reveal significantly stronger relation between the full-disc and the northern hemisphere than between the full-disc and the southern hemisphere while no significant correlations was found between the hemispheres one another.