An identification for GEMINGA: A review of all the available data

Dedicated X-ray, optical and radio observations aimed at the identification of the bright γ-ray source 2CG195+04 (GEMINGA) are presented. A very promising candidate is found and its properties are discussed in the context of possible astrophysical scenarios.     

一种航空图像道路中心线快速提取算法

经典的航空图像道路中心线提取算法针对非实时应用,计算耗时长,难以满足视觉辅助导航、实时地物识别等应用的要求。在研究了图像中道路法向和等效道路宽度的基础上,建立了近似道路法向和等效道路宽度模型来代替经典道路模型,提出了基于道路中心线的快速提取方法。对比实验的结果说明：快速提取方法和经典方法取得了相近的道路提取效果,计算耗时大大下降,可以满足实时性要求。     

The MESSENGER Gamma-Ray and Neutron Spectrometer

A Gamma-Ray and Neutron Spectrometer (GRNS) instrument has been developed as part of the science payload for NASA’s Discovery Program mission to the planet Mercury. Mercury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) launched successfully in 2004 and will journey more than six years before entering Mercury orbit to begin a one-year investigation. The GRNS instrument forms part of the geochemistry investigation and will yield maps of the elemental composition of the planet surface. Major elements include H, O, Na, Mg, Si, Ca, Ti, Fe, K, and Th. The Gamma-Ray Spectrometer (GRS) portion detects gamma-ray emissions in the 0.1- to 10-MeV energy range and achieves an energy resolution of 3.5 keV full-width at half-maximum for ⁶⁰Co (1332 keV). It is the first interplanetary use of a mechanically cooled Ge detector. Special construction techniques provide the necessary thermal isolation to maintain the sensor’s encapsulated detector at cryogenic temperatures (90 K) despite the intense thermal environment. Given the mission constraints, the GRS sensor is necessarily body-mounted to the spacecraft, but the outer housing is equipped with an anticoincidence shield to reduce the background from charged particles. The Neutron Spectrometer (NS) sensor consists of a sandwich of three scintillation detectors working in concert to measure the flux of ejected neutrons in three energy ranges from thermal to ∼7 MeV. The NS is particularly sensitive to H content and will help resolve the composition of Mercury’s polar deposits. This paper provides an overview of the Gamma-Ray and Neutron Spectrometer and describes its science and measurement objectives, the design and operation of the instrument, the ground calibration effort, and a look at some early in-flight data.     

低能自由空气电离室优化设计

借助于空气比释动能的基本定义和概念以及空气比释动能绝对测量的理论方法,分析了自由空气电离室可以作为空气比释动能绝对测量方法的原理和条件。通过平板型与圆柱型自由空气电离室的优劣比较,选择平板型作为研究对象,详细介绍了经典的平板型自由空气电离室,并通过理论分析计算以及模拟计算的方法,优化设计包括:光阑半径、空气衰减长度、极间距等低能自由空气电离室的关键几何尺寸,以最小化空气比释动能测量时产生的总不确定度。     

X射线脉冲星绝对定位法研究

研究和分析了脉冲星定位方法中的绝对定位法。通过一系列的公式和图表详细分析了定位算法的理论依据,同时还对整周模糊度问题的解算进行了研究。最后,利用MATLAB建立了一个简单模型,对定位算法进行仿真。结果表明定位准确度与星载原子钟准确度、脉冲星相位模型准确度以及相位观测误差有直接联系。     

基于MSER的无人机图像建筑区域提取

对建筑区域自动检测与提取是无人机(UAV,Unmanned Aerial Vehicle)图像处理的一项重要功能.在分析无人机成像特点和最大稳定极值区域(MSER,Maximum Stable Extremal Regions)算法对无人机侦察图像建筑区域检测的适用性基础上,提出了一种基于MSER的无人机侦察图像建筑区域提取算法.算法包含5步:无人机图像预处理,运用MSER算法分析计算图像稳定区域,通过计算稳定区域密度筛选建筑区域,进一步利用自适应K均值聚类算法对建筑区进行划分,最后采用Graham算法生成建筑区的边界从而实现了建筑区的自动提取.选取无人机实飞图像数据进行实验统计,本算法提取精度为92.25%;同时与基于Gabor变换的纹理特征、SIFT特征点的提取算法相比,建筑区域提取时间缩短,满足无人机实时应用需求.      

The Burst Alert Telescope (BAT) on the SWIFT Midex Mission

he burst alert telescope (BAT) is one of three instruments on the Swift MIDEX spacecraft to study gamma-ray bursts (GRBs). The BAT first detects the GRB and localizes the burst direction to an accuracy of 1–4 arcmin within 20 s after the start of the event. The GRB trigger initiates an autonomous spacecraft slew to point the two narrow field-of-view (FOV) instruments at the burst location within 20–70 s so to make follow-up X-ray and optical observations. The BAT is a wide-FOV, coded-aperture instrument with a CdZnTe detector plane. The detector plane is composed of 32,768 pieces of CdZnTe (4×4×2 mm), and the coded-aperture mask is composed of ∼52,000 pieces of lead (5×5×1 mm) with a 1-m separation between mask and detector plane. The BAT operates over the 15–150 keV energy range with ∼7 keV resolution, a sensitivity of ∼10⁻⁸ erg s⁻¹ cm⁻², and a 1.4 sr (half-coded) FOV. We expect to detect > 100 GRBs/year for a 2-year mission. The BAT also performs an all-sky hard X-ray survey with a sensitivity of ∼2 m Crab (systematic limit) and it serves as a hard X-ray transient monitor.     

高帧频数字相机在高速流动显示中的应用

根据高速流动显示实验研究对高帧频图像采集设备的需要,基于分幅式光路设计原理,结合快响应像增强器和低照度CCD相机,研制了一套兆赫兹采样的高帧频数字相机。利用高帧频数字相机,开展了高速流动显不实验研究：基于高帧频数字相机,结合纹影技术,在激波管上针对方块、凹槽模型,开展了高速流动显示实验,获取了运动激波与模型边界相互作用的序列图像,观察到湍流涡随时间演化发展的过程。结合一台输出功率为8W的连续激光光源和高帧频数字相机,建立了一套高速片光散射流动显示系统,获取了喷流的米氏散射序列图像。实验证明,基于高帧频数字相机的纹影及片光散射技术具备开展高速流动显示实验研究的能力。     

Relative ionizations in the nearest interstellar gas

We compare CLOUDY predictions for the equilibrium ionization in the interstellar cloud surrounding the solar system with pick-up ion data. The incident radiation field includes contributions from hot stars, the emission from the conductive cloud boundary and the diffuse FUV back-ground. To within the observational uncertainties, CLOUDY predictions for the ratios n(He)/n(O), n(N)/n(O), n(Ne)/n(O), and n(He)/n(Ne) are consistent with pick-up ion data, provided that O and N are filtered by 50% in the heliopause region and the outer heliosphere as predicted by others. Thus, the steady-state ionization model and assumed radiation field appear approximately valid. However, the youth and low intervening column density towards the Vela pulsar leave open the possibility that the parent supernova explosion 10,500 years ago, and 200 pc distant, may also have affected LISM ionization, although the mechanism is uncertain. Support for this last possibility is provided by the apparent signature of the Vela explosion in the terrestrial geological record.Abbreviations ISM Interstellar Medium - FUV Far Ultraviolet - EUV Extreme Ultraviolet - SNR SN remnant - SXRB SXR Background - LISM Local Interstellar Matter     

稀土钇提高离子镀TiN膜层与基体结合力的研究

研究了稀土钇不同含量时对离子镀ＴｉＮ膜层与基体结合力的影响．用扫描电镜，俄歇谱仪，Ｘ射线衍射等手段，对加入稀土钇的ＴｉＮ膜层作了分析。结果表明，加适量稀土钇后，ＴｉＮ膜层与基体的结合力大大提高。其微观机制是，加稀土钇后，膜层相组成发生变化，在膜－基之间形成一过渡层，塑性相（Ｔｉ相）增加，脆性相（Ｔｉ２Ｎ）减少，从而减小了膜－基界面间的应力。此外，结果还表明，稀土钇能明显提高镀膜过程中钛料蒸发率，使成膜速率增加，在相同镀膜时间内ＴｉＮ膜层加厚。