我国海洋声学探测技术竞争力分析

海洋声学探测技术用于海洋物理及海洋特定目标特性探测,是人类认识海洋、开发和利用海洋丰富资源必不可少的海洋高技术。文中全面介绍了海洋声学探测技术的技术结构以及致力于此技术研究的国内外主要研究机构,着重对比分析了国内外海洋声学探测技术的发展现状与趋势,并总结出我国该领域现存在的问题。结果表明我国海洋声学探测技术水平与国外相差10 a左右,未来需靠长期稳定支持、按需开展研究、加大基础工业投资以及提高材料与工艺水平等措施推进我国海洋声学技术的良性发展。     

轨道扣件病害自动化检测研究及应用

传统扣件检查基本采用人工检查方式,不仅工作效率低、劳动强度大,而且人为干扰因素多、检查采样率低。针对以上问题,本文提出了一种基于线结构光传感器的轨道扣件损伤和松动检测方法,并开发了轨道扣件智能监测系统以实现扣件病害自动检测。最终将研究成果应用于徐州市某地铁区间轨道扣件检测,验证了该方法的可行性和准确率,为地铁轨道扣件检查提供了新方法。     

基于卷积神经网络的无人机影像违章建筑检测应用

无人机航拍影像具有分辨率高、回访周期短等特点,利用无人机遥感技术手段对城市范围的建设进行动态监测,可及时、有效地发现涉嫌违法的建设活动。本文结合实际项目需求,研究通过卷积神经网络方法进行违章建筑的自动检测,替代过去靠大量人力检查的模式,目前测试区域无人机影像试验取得了较好的效果,在样本数据不足5000份的情况下,准确率和召回率分别达到了71%和88%。随着样本数据的不断增多,基于该深度学习方法将较大程度上持续提升检测准确率和召回率,能够更精准地发现违法活动,具有较大的实际应用价值及潜力。     

利用结构面对象的高分遥感影像建筑物变化检测

根据建筑物具有丰富的角点和规则的外观形状的特点,本文提出了依据线段信息生成建筑物变化检测基本单元——结构面对象的建筑物变化检测方法。从高分遥感影像中提取出建筑物的边缘线及屋顶外形线条,生成结构面对象并提取其在两时相影像中相应的特征信息,通过监督分类获取变化建筑区域。试验结果表明,利用结构面对象进行建筑物变化检测能较完整地覆盖变化建筑物表面且对象边缘检测效果较好。     

基于点云投影线探测的高墩位姿自动检测方法

针对目前超高桥墩垂直度检测方法存在危险系数较高、精度难以保证或自动化程度与工作效率较低的情况,本文提出一种基于三维激光扫描技术的点云数据超高桥墩位姿自动检测方法。该方法首先将海量墩面点云双向分层;然后依条件选择分层文件探测点云投影线并划分桥墩面缓冲区;最后根据缓冲区自动提取墩面点云并进行位姿检测。本文以某山区高速桥梁高墩位姿检测为例进行试验,试验结果,表明该方法具有无接触测量、高自动化、高工作效率及检测范围全面的优势。     

地面自动气象观测设备运行状态信息检测技术

地面自动气象观测设备运行状态检测机制不足一直是困扰我国地面气象观测运行保障工作的一大难题。本研究从运行监控实际业务需求角度出发,在梳理现有业务运行地面自动气象观测设备结构基础上,结合部分研究成果,从数据采集模块、气压观测模块、温湿度观测模块、风观测模块、地温观测模块、雨量观测模块、供电系统模块、软件模块、能见度观测模块和称重降水观测模块共10个方面逐一细化了每一主要部件的状态检测点,并对其进行了分类和编码,同时参考现行业务运行设备长Z数据报文,制定了地面自动气象观测设备运行状态报文规范,最终研制了地面自动气象观测设备运行状态信息检测技术。通过统一规范、标准,研究结果可解决目前我国地面自动气象观测设备监控信息设计规范缺失的问题,可缓解当前厂家多、型号杂、设备不统一的不利局面,有利于推进地面自动气象观测设备运行监控技术规范化建设工作。     

On the use of X-ray and γ-ray telescopes for identifying the origin of electrons and positrons observed by ATIC, Fermi, and PAMELA

X-ray and γ-ray observations can help understand the origin of the electron and positron signals reported by ATIC, PAMELA, PPB-BETS, and Fermi. It remains unclear whether the observed high-energy electrons and positrons are produced by relic particles, or by some astrophysical sources. To distinguish between the two possibilities, one can compare the electron population in the local neighborhood with that in the dwarf spheroidal galaxies, which are not expected to host as many pulsars and other astrophysical sources. This can be accomplished using X-ray and γ-ray observations of dwarf spheroidal galaxies. Assuming the signal detected by Fermi and ATIC comes from dark matter and using the inferred dark matter profile of the Draco dwarf spheroidal galaxy as an example, we calculate the photon spectrum produced by electrons via inverse Compton scattering. Since little is known about the magnetic fields in dwarf spheroidal galaxies, we consider the propagation of charged particles with and without diffusion. Extending the analysis of Fermi collaboration for Draco, we find that for a halo mass ∼10⁹ M_⊙, even in the absence of diffusion, the γ-ray signal would be above the upper limits. This conclusion is subject to uncertainties associated with the halo mass. If dwarf spheroidal galaxies host local magnetic fields, the diffusion of the electrons can result in a signal detectable by future X-ray telescopes.     

Optimized running conditions and sensitivity for direction sensitive detectors of WIMP dark matter

Optimum fill pressures for direction-sensitive dark matter detectors based on tracking in gases are considered. Given the minimum resolvable track length and the gas fill, the Lindhard–Scharf stopping model leads to the existence of an optimum pressure which maximizes the specific event rate R (event rate per unit detector volume). In addition, maximizing the detectibility of the recoil nucleus diurnal asymmetry is considered. Optimum fill pressures are calculated for Ar, CF₄, CS₂ and Xe gas fills, as a function of the WIMP mass and the minimum resolvable track length. The associated minimum target volumes required to achieve currently competitive WIMP-nucleon cross-section sensitivity are also calculated. The standard isothermal sphere model of the galactic WIMP halo is used throughout, but the method could be extended to use any desired WIMP distribution function.     

Detection and Correction of AMSR-E Radio-Frequency Interference

Radio-frequency interference (RFI) affects greatly the quality of the data and retrieval products from space-borne microwave radiometry. Analysis of the Advanced Microwave Scanning Radiometer on the Earth Observing System (AMSR-E) Aqua satellite observations reveals very strong and widespread RFI contam- inations on the C- and X-band data. Fortunately, the strong and moderate RFI signals can be easily identified using an index on observed brightness temperature spectrum. It is the weak RFI that is diffi- cult to be separated from the nature surface emission. In this study, a new algorithm is proposed for RFI detection and correction. The simulated brightness temperature is used as a background signal (B) and a departure of the observation from the background (O-B) is utilized for detection of RFI. It is found that the O-B departure can result from either a natural event (e.g., precipitation or flooding) or an RFI signal. A separation between the nature event and RFI is further realized based on the scattering index (SI). A positive SI index and low brightness temperatures at high frequencies indicate precipitation. In the RFI correction, a relationship between AMSR-E measurements at 10.65 GHz and those at 18.7 or 6.925 GHz is first developed using the AMSR-E training data sets under RFI-free conditions. Contamination of AMSR-E measurements at 10.65 GHz is then predicted from the RFI-free measurements at 18.7 or 6.925 GHz using this relationship. It is shown that AMSR-E measurements with the RFI-correction algorithm have better agreement with simulations in a variety of surface conditions.     

2.4m望远镜网络安全初步设计

云南天文台将在2.4m望远镜建立远程观测系统。由于远程观测系统通过网络实现通信,必然会面临网络上的各种威胁。为了保证整个网络系统的安全,避免各种不安全因素造成的损失。在对现在望远镜网络分析基础上设计了安全的网络结构,并实现了具有入侵检测功能的防火墙,这些措施初步保障了2.4m望远镜网络系统的安全。