基于分段化结构重建的2D/3D视频转换方法

为了缓解3D片源的不足,设计了一种分段化结构重建方法为视频2D/3D转换提供深度线索.采用分层提取的方式,将视频基于内容分解为子序列,在每个子序列中建立优化准则选择出处于非退化状态的关键帧,并以此为基础提出了分段化结构重建框架,利用改进的耦合自标定算法重构出每个子序列对应的离散3D结构信息,从而获取视频的深度线索.实验结果表明,该方法通过分段化后的局部优化,不仅使结构化重建能够有效处理多场景下的连续镜头,还加快了转换的效率,能够稳定、高效地获取深度信息,适用于视频2D/3D转换.      

分离式机械压汽蒸馏系统的实验

针对传统机械压汽蒸馏的不足,提出分离式机械压汽蒸馏系统.建立了一套容量为1.5 m3/d的单效分离式机械压汽蒸馏系统并对其进行实验研究.实验系统主要由两套旋转蒸发器、冷凝器以及压缩机组成.通过改变压缩机转速和蒸发温度来研究系统的性能.结果表明在蒸馏水产量一定的前提下压缩机进口压力和冷凝器进口压力随着压缩机转速的增加而逐渐下降,换热温差随着压缩机转速的增加而增加,最高温差稳定在8.5℃左右.通过改变系统的真空度获得不同的蒸发温度,蒸发温度越高,蒸馏产量越高,系统性能也越好.      

面向数字化技术支援的数字样机逐层轻量化技术

直观的三维模型有助于提高民用飞机远程维修支援的效率和准确度,但由于计算机辅助设计系统产生的模型数据量通常比较巨大,三维数字样机的轻量化成为了很大的挑战.基于对格式转换与模型简化这两种轻量化方法的分析,提出了基于单元数据量的数字样机逐级轻量化的方法,将全机的三维模型进行不同简化程度的轻量化处理,并且提出了基于失真度判据的层级化管理方法,按照模型结构树对简化率高的失真模型与具有细节特征的无损模型进行逐级的加载与使用.实例验证表明所提出的方法有效减小了网络传输的数据量并保留了模型必要的细节特征,使在互联网中快速访问全机三维模型得以实现.     

气动负载模拟器的多余力矩分析

为了分析气动负载模拟器中多余力的形成及影响因素,介绍了气动负载模拟器的工作原理、结构框图及实验平台,推导了气动负载模拟器的数学模型,并通过实验和仿真对比模型进行了验证。采用线性化方法定性分析了影响气动负载模拟器多余力的3个因素——被动压差、惯性力矩以及摩擦力矩。采用非线性仿真定量分析了该3个因素分别对气动负载模拟器的多余力矩的影响。得出了在气动伺服加载系统中,摩擦力矩是引起系统多余力矩的重要因素。     

基于欧拉法模拟旋转帽罩水滴撞击特性

基于欧拉两相流理论,对旋转帽罩水滴撞击特性进行了数值模拟。通过引入耗散函数求解水滴相无黏欧拉方程,实现了欧拉法求解三维旋转帽罩的水滴撞击特性。分析了旋转帽罩转速对水滴撞击特性的影响。发现旋转帽罩转速越大,其表面水滴撞击极限稍有减小。在典型飞行条件与气象条件下,离心力对水滴运动轨迹的影响远小于惯性力对其的影响,旋转帽罩转速对水滴撞击特性影响较小。     

A 3NM-64_He added to LARC for Solar Extreme Event studies during solar cycle 24

The Antarctic Laboratory for Cosmic Rays (LARC, acronym for Laboratorio Antartico per i Raggi Cosmici or Laboratorio Antártico para Rayos Cósmicos) operates on King George Island (South Shetlands). Since January 1991 a standard 6NM-64 detector has been recording continuous cosmic ray measurements and several Ground-Level Enhancements have been registered. Here we describe the different phases performed in Italy for the realization of a 3NM-64_³He detector, which started its measurements during the Italian XXII Antarctic Summer Campaign. Data recorded during solar activity cycle 24 will furnish an useful research tool for the next Solar Extreme Events.     

Orbital phase spectroscopy of four high mass X-ray binary pulsars to study the stellar wind of the companion

Our work focuses on a comprehensive orbital phase-dependent spectroscopy of the four High Mass X-ray Binary Pulsars (HMXBPs) 4U 1538-52, GX 301-2, OAO 1657-415 and Vela X-1. We hereby report the measurements of the variation of the absorption column density and iron-line flux along with other spectral parameters over the binary orbit for the above-mentioned HMXBPs in elliptical orbits, as observed with the Rossi X-ray Timing Explorer (RXTE) and the BeppoSAX satellites. A spherically symmetric wind profile was used as a model to compare the observed column density variations. Out of the four pulsars, only in 4U 1538-52, we find the model having a reasonable corroboration with the observations, whereas in the remaining three the stellar wind seems to be clumpy and a smooth symmetric stellar wind model appears to be quite inadequate in explaining the data. Moreover, in GX 301-2, neither the presence of a disk nor a gas stream from the companion was validated. Furthermore, the spectral results obtained in the case of OAO 1657-415 and Vela X-1 were more or less similar to that of GX 301-2.     

Coronal fast wave trains of the decimetric type IV radio event observed during the decay phase of the June 6, 2000 flare

The 22 min long decimetric type IV radio event observed during the decay phase of the June 6, 2000 flare simultaneously by the Brazilian Solar Spectroscope (BSS) and the Ond?ejov radiospectrograph in frequency range 1200–4500 MHz has been analyzed. We have found that the characteristic periods of about 60 s belong to the long-period spectral component of the fast wave trains with a tadpole pattern in their wavelet power spectra. We have detected these trains in the whole frequency range 1200–4500 MHz. The behavior of individual wave trains at lower frequencies is different from that at higher frequencies. These individual wave trains have some common as well as different properties. In this paper, we focus on two examples of wave trains in a loop segment and the main statistical parameters in their wavelet power and global spectra are studied and discussed.     

The acceleration of Anomalous Cosmic Rays by stochastic acceleration in the heliosheath

Stochastic acceleration in the heliosheath appears to be a likely mechanism by which Anomalous Cosmic Rays (ACRs) are accelerated. However, most stochastic acceleration mechanisms are not appropriate. The energy density in the ACRs and in the interstellar pickup ions out of which the ACRs are accelerated greatly exceeds the energy density in the turbulence in the heliosheath. Thus, a traditional stochastic acceleration mechanism in which particles are accelerated by damping the turbulence will not work. A stochastic acceleration mechanism has been developed in which the total energy of the pickup ions and the ACRs is conserved. Energy is redistributed from the core pickup ions into a suprathermal tail to create the ACRs. A model for the acceleration of the ACRs in the heliosheath, based on this stochastic acceleration mechanism, is presented. The model provides reasonable fits to the spectra of suprathermal particles and ACRs observed by Voyager.