X-ray imaging techniques— modulation collimator and coded mask

Imaging over the hard X-ray energy band may be achieved by masking the flux with proper obstacles. The imaging modulation collimator has been developed and has been applied thus far, e.g., to produce hard X-ray pictures of the solar flare and to construct the X-ray image of the Crab Nebula up to the angular resolution of ～ 10 arcsec. Variations of the concept such as the Fourier Transform Telescope are discussed. Virtue of the modulation collimator is that high angular resolution may be achieved with a relatively simple detector system and that a wide field of view may be accomodated. Among several proposed coded masks, the techniques of Hadamard transform are discussed in some details. The coded mask is provided with a better total transmission, but its angular resolution is limited due to presently limited spatial resolution of the detector. Developments of the technique of the position sensitive detector are awaited for further improvements of the resolution.     

Energetic positive ions in the cometary “foreshock” region

Ions produced by ionization of the cometary neutrals interact with the solar wind protons to produce large amplitude oscillations of the ambient magnetic field. Such oscillations are convected towards the comet at the unperturbed solar wind speed far from the shock and at a lower speed closer to the shock (due to the solar wind mass loading); hence, they can energize the incoming ions by Fermi acceleration. The spatial extension of the acceleration region is of the order of 10⁶ km and the resulting energy spectrum is harder than in the Earth's bow shock case. The energization of cometary ions produces an additional deceleration of the solar wind. It is suggested that Comet Halley may be the most efficient “cosmic ray shock” in the solar system.     

Ablation and chemistry of meteoric materials in the atmosphere of Titan

We compute the input of meteoric materials expected on Titan, and integrate this dust model with an ablation model and a comprehensive chemical model, investigating the effects on the atmosphere and surface. We find that a water deposition of 10-100 times the expected interplanetary dust flux /7/, or a recent large impact, is required to produce the observed CO₂ abundance /2/. Ionisation due to meteoric activity is not likely to be higher than that due to other sources.     

基于薄膜热电堆的新型高温瞬态热流密度传感器的研制

目前针对国内薄膜瞬态热流传感器一致性较差、制备工艺不成熟等问题，提出了一种基于光刻工艺和离子束溅射镀膜工艺的制备方法，200对T型金属薄膜热电偶沉积在10mm×10mm的水冷块上，测量1μm的氧化铝热阻层温差，从而得到瞬态热流密度值。对新型高温瞬态热流密度传感器进行比对法标定，一致性误差为0.211%，即工艺的一致性约为99.79%。实验表明，研制的新型高温瞬态热流密度传感器的一致性好,制备工艺具备良好重复性和可移植性，能够满足高温瞬态热流检测需要，为热流传感器的推广应用及标准化、批量化生产提供了良好的技术支撑。     

基于薄膜热电堆的新型高温瞬态热流密度传感器的研制

目前针对国内薄膜瞬态热流传感器一致性较差、制备工艺不成熟等问题，提出了一种基于光刻工艺和离子束溅射镀膜工艺的制备方法，200对T型金属薄膜热电偶沉积在10mm×10mm的水冷块上，测量1μm的氧化铝热阻层温差，从而得到瞬态热流密度值。对新型高温瞬态热流密度传感器进行比对法标定，一致性误差为0.211%，即工艺的一致性约为99.79%。实验表明，研制的新型高温瞬态热流密度传感器的一致性好,制备工艺具备良好重复性和可移植性，能够满足高温瞬态热流检测需要，为热流传感器的推广应用及标准化、批量化生产提供了良好的技术支撑。     

氧化锌色素在真空紫外辐照下降解机理的研究

研究氧化锌色素在真空紫外辐照下的降解机理,目的是为设计在宽间环境下稳定的氧化锌热涂层提供理论依据。仔细研究了自由电子在氧化锌中的吸收特性及真空紫外辐照对氧化锌电导的贡献,认为真空紫外辐照引起氧化锌色素表面化学吸附氧的解析,同时在氧化锌色素表面产生大量的氧空位,氧空位提供了导带中的自由电子,自由电子在导带内跃迁吸收近红外光子引起氧化锌色素光学性能的退化。     

Models of CNS radiation damage during space flight.

The primary structural and functional arrangement of the different cell types within the CNS are reviewed. This was undertaken with a view to providing a better understanding of the complex interrelationships that may contribute to the pathogenesis of lesions in this tissue after exposure to ionizing radiation. The spectrum of possible CNS radiation-induced syndromes are discussed although not all have an immediate relevance to exposure during space flight. The specific characteristics of the lesions observed would appear to be dose related. Very high doses may produce an acute CNS syndrome that can cause death. Of the delayed lesions, selective coagulation necrosis of white matter and a later appearing vascular microangiopathy, have been reported in patients after cancer therapy doses. Lower doses, perhaps very low doses, may produce a delayed generalised CNS atrophy; this effect and the probability of the induction of CNS tumors could potentially have the greatest significance for space flight.     

一种基于攻击距离的对抗样本攻击组筛选方法

黑盒对抗样本生成过程中通常会指定1个攻击组，包括1个原始样本和1个目标样本，使得生成的对抗样本与原始样本范数差别不大，但被分类器识别为目标样本的分类。针对攻击组的攻击难度不同导致攻击不稳定的问题，以图像识别领域为例，设计了基于决策边界长度的攻击距离度量方法，为攻击组的攻击难易程度提供了度量方法。在此基础上，设计了基于攻击距离的对抗样本攻击组筛选方法，在攻击开始前就筛去难以攻击的攻击组，从而实现在不修改攻击算法的前提下，提升攻击效果。实验表明:相比于筛选前的攻击组，筛选后的攻击组的总体效果提升了42.07%，攻击效率提升了24.99%，方差降低了76.23%。利用攻击组的对抗样本生成方法在攻击前先进行攻击组筛选，可以稳定并提高攻击效果。      

SPOT image quality and post-launch assessment

In this paper we present the image quality specifications for the SPOT System and the methods used for their assessment. These methods fall into two categories: pre-launch ground testing and post-launch assessment (during the satellite's first two months in orbit). The geometric specifications concern image location accuracy, length distortion, anisomorphism, multi-date and multispectral registration, local coherence and, in the case of stereo pairs, accuracy of elevation measurement. The radiometric specifications concern: signal-to-noise ratio, detector equalization and array response linearity; band-to-band, absolute and multi-date registration; distortion due to high radiances (blooming) and modulation transfer function (MTF).     

How far are we from a ‘Standard Model’ of the solar dynamo?

Over the last few years, dynamo theorists seem to be converging on a basic scenario as to how the solar dynamo operates. The strong toroidal component of the magnetic field is produced in the tachocline, from where it rises due to magnetic buoyancy to produce active regions at the solar surface. The decay of tilted bipolar active regions at the surface gives rise to the poloidal component, which is first advected poleward by the meridional circulation and then taken below the surface to the tachocline where it can be stretched to produce the toroidal component. The mathematical formulation of this basic model, however, involves the specification of some parameters which are still uncertain. We review these remaining uncertainties which have resulted in disagreements amongst various research groups and have made it impossible to still arrive at something that can be called a standard model of the solar dynamo.     

一种带移动副平面六连杆机构分支识别方法

带移动副平面六连杆机构的分支、运动缺陷、运动范围等的判别是机构运动特性研究的重要指标。首先,将带2个移动副或3个移动副的平面六连杆机构分为四环链及五环链,引入欧拉公式、三角换元等方法,得到带移动副机构在极限位置（包括死点、分支点）的具体构型、具体关节输入输出关系以及关节旋转空间。其次,将2个链路结合,提出带2个移动副及3个移动副平面六连杆机构的分支识别方法。最后,通过实例验证,得到机构的分支点、死点及关节在所有极限位置的具体角度,为带移动副机构分支的自动识别提供了一种简便有效的方法。      

Energy balance in solar active regions: The dip of April, 1985

The presence of a solar active region affects the luminosity of the sun. Sunspots directly produce “dips” in the total solar irradiance approximately proportionally to their projected area, while faculae produce excess energy. These effects were discovered during the solar maximum period of 1980, and in this paper we examine the sunspot effect during solar minimum. We examine the “dip” due to an active region in April, 1985, as observed in the total solar irradiance by the ACRIM instrument on the Solar Maximum Mission. These data (obtained after the spacecraft repair in May, 1984) have simple variations, relative to those observed in 1980, because of the reduced level of activity approaching solar minimum. We find that the PSI index of projected sunspot area as defined in 1980 appears to describe this “dip” satisfactorily.     

日冕环和日冕拱的平衡位形

在线性场近似条件下,本文讨论了日冕环的二维平衡位形。用富利叶变换的方法,求出了问题的分析解,解释了日冕环观测结果的主要特性。沿日冕环纵向的压力分布均匀,日冕环的位形可以比无力场更稳定。由于日冕环可以储存更多的剪切场或扭转场的磁能,释放这部分磁能就可以驱动日冕环运动产生日冕瞬变过程,或者使环内的等离子体加热或加速而产生太阳耀斑。      

太阳米波噪暴：哨声模式

本文以日冕活动区磁结构演化为噪暴现象的驱动力,并假定日冕活动区在磁学上是不均匀的——存在强磁场纤维,提出了太阳米波噪暴的哨声模式.活动区磁结构的演化将在冕弧中产生弱激波.当弱激波通过强磁场纤维时,加热部分电子,被加热的电子在强磁场纤维中形成损失锥分布.在日冕的噪暴区域中,快速电子的损失锥分布将产生高亮度的哨声波和朗缪尔波.通过感应散射,朗缪尔波滑向低波区域时将与哨声波发生强烈的互作用而产生窄束电磁辐射(Ⅰ型爆发).强磁场纤维及相应的场位形决定了Ⅰ型爆发的频宽和持续时间.而噪暴连续谱则采用通常认为的各同向电子产生的朗缪尔波与低频波耦合的产物.     

Radiation chemistry of the hippocampal brain slice.

The in vitro hippocampal brain slice is a 0.4 mm thick neural network that can be used to study brain responses to radiation and related injuries. This preparation is unique in that it responds to ionizing radiation within minutes after exposure without complications from changes in vascularity, blood flow, blood pressure, etc. Electrophysiological studies have shown that x- and gamma-rays alter synaptic transmission and spike generation, elements of normal brain activity. To evaluate the role of hydroxyl free radicals (OH) in these changes, slices were exposed to dilute H2O2 solutions. EPR spin trapping experiments verified that OH is produced. Neural responses, while similar, were not identical to those due to radiation, possibly because of a different distribution of OH. Although H2O2 is freely diffusible, it produces OH at specific sites where, e.g. iron reduces it. In contrast, x- and gamma-rays produce OH more uniformly throughout the tissue. H2O2 may provide a better model for high-LET radiation where yields of radical products of water radiolysis are decreased and peroxide reactions predominate.     

啁啾脉冲激光放大系统中的色散研究

理论分析了飞秒钛蓝宝石激光啁啾脉冲放大系统中各光学元件引入的色散,讨论了以块状玻璃作为展宽器,以双棱镜对作为压缩器的应用,并以重火石玻璃ZF7为基材,模拟了展宽--放大--压缩过程中脉冲宽度的变化。相较于光栅对展宽器来说,光学玻璃的展宽倍数较小,但是对于放大能量不高的预放大系统来说,这种展宽--压缩方式价格低廉、调节简便,具有较大的应用价值。通过灵活的选择基底玻璃材料及调节棱镜的插入量,或者将该展宽--压缩系统与光栅对及高阶色散啁啾镜混合使用,实现优势互补,可以进一步补偿高阶色散,缩短压缩脉冲宽度。     

火星进入段探测器自校准状态估计

由于大气密度、气动参数、突风和沙尘暴等因素的影响,火星探测器在进入段高速飞行的动力学模型中往往带来未知输入,这些未知输入使传统的滤波方法出现较大的偏差。研究采用一种新的自校准扩展Kalman滤波方法,对火星进入段的探测器进行状态估计,可以成功地消除这些未知输入带来的影响。数值仿真结果表明,该方法能有效提高导航精度。     

Estimating low resolution gravity fields at short time intervals to reduce temporal aliasing errors

The Gravity Recovery and Climate Experiment (GRACE) satellite mission has been estimating temporal changes in the Earth’s gravitational field since its launch in 2002. While it is not yet fully resolved what the limiting source of error is for GRACE, studies on future missions have shown that temporal aliasing errors due to undersampling signals of interest (such as hydrological variations) and errors in atmospheric, ocean, and tide models will be a limiting source of error for missions taking advantage of improved technologies (flying drag-free with a laser interferometer). This paper explores the option of reducing the effects of temporal aliasing errors by directly estimating low degree and order gravity fields at short time intervals, ultimately resulting in data products with improved spatial resolution. Three potential architectures are considered: a single pair of polar orbiting satellites, two pairs of polar orbiting satellites, and a polar orbiting pair of satellites coupled with a lower inclined pair of satellites. Results show that improvements in spatial resolution are obtained when one estimates a low resolution gravity field every two days for the case of a single pair of satellites, and every day for the case of two polar pairs of satellites. However, the spatial resolution for these cases is still lower than that provided by simply destriping and smoothing the solutions via standard GRACE post-processing techniques. Alternately, estimating daily gravity fields for the case of a polar pair of satellites coupled with a lower inclined pair results in solutions with superior spatial resolution than that offered by simply destriping and smoothing the solutions.     

基于三维点云模型的空间目标光学图像生成技术

空间探测任务中大量先验图像数据的缺乏，使得基于光学图像的态势感知和导航算法无法被有效定量测试和评估。针对此问题，提出了一种基于三维点云模型和射影变换基本理论的空间目标光学图像生成方法。在完成对空间目标三维点云模型和仿真摄像机模型构建基础之上，利用射影变换基本理论依次计算像平面所有像素点与空间目标三维点云模型空间点的对应关系，并基于Lambertian漫反射模型和相对应空间目标三维点云模型空间点的光照方向，得到所有像素点的灰度值，从而生成给定空间目标的光学图像。大量仿真实验表明:与传统的基于解析模型的仿真图像生成方法相比，所提的空间目标光学图像生成技术能够以更快的速度生成更加真实的仿真图像，且生成的仿真图像可以广泛应用于椭圆拟合、陨石坑检测、着陆器视觉导航、航天器交会对接、空间目标跟踪等典型空间应用算法的定性与定量评估。      

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.