时间频率设备自动监控系统的设计与实现CSCD

针对时间频率实验室设备实时监控的需求,在Microsoft NET平台上结合C++语言和Microsoft SQL server数据库技术,构建了时间频率设备自动监控系统。该系统可以实时监测设备的运行状态,并远程设置相关参数,在设备运行异常时,系统可自动弹出报警信息。实际应用表明系统具有较好的实用性、可维护性,为时间频率实验室的有序运行提供了保障。     

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.     

SVIRCO contribution to the world-wide network of cosmic ray detectors

Since 1954 a research team (called SVIRCO) has been performing measurements of cosmic rays in Rome at La Sapienza University till 1997 and then at Roma Tre University. The experimental work carried out over more than 50 years is summarized in this paper. It describes: the early history of SVIRCO, the evolution from SVIRCO station to SVIRCO observatory, land and sea cosmic-ray surveys and the mini-network of neutron monitors, operating inside the world-wide network of cosmic ray detectors.     

考虑膨胀效应的UH模型及其有限元实现

超固结非饱和土统一硬化(UH)模型在分析超固结非饱和土问题中有广泛的适用性,其不仅可以使超固结状态下的湿化模拟更为合理,也能够反映超固结非饱和土的硬化、软化等特性。在超固结非饱和土本构模型的基础上,考虑土体团粒的吸水膨胀作用,提出了考虑膨胀效应的UH模型。该模型只比超固结非饱和土UH模型增加了一个参数,不仅能够描述普通加载路径下超固结膨润土的应力应变特性,还能反映其在湿化路径下的膨胀效应。基于有限元软件的二次开发平台,进行了考虑膨润土膨胀效应UH模型的有限元实现,并通过对三轴试验和膨胀力试验的数值模拟,验证了模型子程序的合理性。      

航天器相对导航与控制技术的典型任务

在空间交会对接、在轨服务、近距离目标监视以及航天器编队飞行任务中,通常需要通过相对导航与控制技术对相互邻近的航天器进行控制.回顾了该领域典型的空间任务,特别关注任务、相对导航与控制方法、相对测量设备、推进系统等主要特征,并总结了该项技术的发展趋势.     

基于预测碰撞点的剩余飞行时间估计方法

分别针对顺轨与逆轨拦截飞行轨迹的特点,设计了相应的剩余飞行时间（TGO）估计方法。该方法通过对弹目碰撞点的预测,降低了发射条件差异对TGO估计精度的影响。首先对线性比例导引运动方程进行变形,得到拦截弹飞行轨迹关于弹目距离的一阶微分方程,基于预测碰撞点,对不同初始发射角造成的积分结果误差进行修正,得出了2种拦截模式下的TGO解析表达式。通过与3种现有估计方法对比分析,验证了提出方法的实时性和估计精度,且能够优化制导性能。