关于"长河二号"导航系统的时间同步及授时

对“长河二号“导航系统的时间同步及快速恢复等问题作了讨论,提出了利用BPL长波信号、GPS共视或搬运钟等方法来实现时间同步和增加授时功能的方案.最后,给出了“长河二号“东海台链的主台信号与国家授时中心的UTC(NTSC)之间的同步实验结果.     

电视时间同步的可用性

本文综述了利用电视信号作时间、频率同步的各种技术和可能达到的精度，以及存在的一些问题和改进意见．     

利用同步卫星进行中日双向时间传递

时间同步是高精度授时不可缺少的环节。利用同步卫星进行双向时间传递可最大限度地消除路径因素对时间同步的影响,并且可准确,适时地得到高精度的比对结果。国际计量局（ＢＩＰＭ）为改善世界范围内时间同步,提出了全球双向卫星时间传递（ＴＷＳＴＴ）计划。由中国科学院陕西天文台（ＣＳＡＯ）和日本邮政省通信综合研究所（ＧＲＬ）所进行的双向卫星时间传递经过一年的工作,已经得到了较好结果,进一步的分析正在进行中。     

基于DP83640硬件辅助的IEEE1588研究及实现

随着高精度时间同步的广泛应用,采用硬件辅助的IEEE1588协议已成为减少同步误差提高同步精度的理想途径。分析了DP83640物理层芯片的功能结构与IEEE1588时间同步基本原理,构建了以DP83640为主要组成部分的时钟同步功能模块,验证了同步过程。实验及分析表明,在局域网内采用DP83640硬件辅助的IEEE1588协议同步精度可达到纳秒量级。     

上海天文台激光测距站的时频系统

本叙述了上海天台人卫激光测距站的时频系统。随着测距精度的提高，时频系统也要不断地加以改进，包括频率标准和时间同步技术。     

共视法和综合法的GPS时间同步精度比较

对共视法和综合法的GPS时间比对对得到的两地协调世界的时间同步精度进行了比较,两种方法各有特点,都有实用价值,严格共视的GPS时间同步精度为5－10ns,不严格共视的GPS的时间同步精度为10－20ns,综合的GPS时间同步精度为6－12ns.     

Loran—C和GPS国际时间比对的长期结果比较

根据1990－1994年上海天台（SO）和世界上一些时间中心（国际计量局（BIPM）时间部、美国海军天台（USNO））的时间公报公布的数据，对两种时间传递技术（Loran-C和GPS）确定的国际时间同步的长期结果进行了比较分析。SO时间实验室得到如下一些结果：1、1990－1992年，由Loran-C时间传递技术确定的结果表明：系统差约为600ns，不确定度约为90ns(1σ），准确度估计优于1μs。2、1993－1994年，由GPS时间传递技术确定的结果表明：系统差优于30ns，不确定度约为15ns(1σ），准确度估计优于100ns。这些比较结果充分说明了GPS时间传递技术在国际高水平时间同步的中必须有广泛的应用。     

B码设备中的GPS时间信号接口

ＰＯ９７型ＧＰＳ／Ｂ码解调器把ＧＰＳ技术融入Ｂ码设备中,用于自动定时定位和精密时间同步。该设备的ＧＰＳ时码接口解出ＧＰＳ时间信号,并同步所有的时标信号和时间码信号。主要介绍了该接口的硬件和软件的实现过程。     

一种高精度时间同步器的研制与性能测试

针对移动通信网络基站间需要建立高精度时间同步的需求,研制了一种具有高精度时间同步功能和高精度频率输出的时间同步器,并设计了相应的性能测试方法。测试结果表明,在同等条件下,不同时间同步器输出的1PPS平均同步精度优于5ns／d,24h内输出的频率准确度优于10^-12／s,其他各项指标基本合格,符合设计要求。     

基于W500的NTP时间服务器设计

针对局域网领域对时间同步的要求,主要利用微控制器STM32和单片网络接口芯片W5100为核心搭建硬件平台来设计一个高精度、高吞吐量的NTP时间服务器系统,为客户端提供高精度的时间信息,从而实现客户端与服务器时间同步的功能。实验及分析表明,该系统运行稳定,能够实现网络时间同步。     

"日中乌"辨析

从观测资料可认证史载“日中乌”是指太阳黑子,而“阳乌载日”则是日全食时的日冕。二者并非神话,而是写实文字。     

SiS in Orion-KL: evidence for "outflow" chemistry

SiS has been conclusively detected toward Orion-KL via its J = 6-5 and J = 5-4 rotational transitions at 91 and 109 GHz. Line profiles indicate that the species is present at an LSR velocity of 7.5 km s-1 with a half-width at zero power of 36 km s-1. Such characteristics associate SiS with the moderate velocity outflow (V approximately 18 km s-1) centered on IRc2 and observed in thermal SiO, the NH3 "plateau," and OH, H2O, and SiO masers. The column density estimated for SiS in this region is Ntot = 4 x 10(15) cm-2, corresponding to a fractional abundance of f approximately 4 x 10(-9). Such an abundance implies an SiO/SiS ratio of approximately 60 in the outflow material, remarkably close to the cosmic O/S ratio of approximately 40 and contrasting with the SiO/SiS value of > approximately 10(3) predicted by ion-molecule models. This difference is probably a result of the high temperatures and densities present in the outflow, which favor thermal equilibrium abundances similar to those observed in the circumstellar shells of late-type stars rather than "ion-molecule"-type concentrations. In addition to SiS, some twenty new unidentified lines near 91 and 109 GHz were detected toward KL, as well as transitions arising from HC5N, HC13CCN, HCC13CN, O13CS, and, possibly, CH3CH2OH, CH3CHO, and CH3OD.     

“Small Equipment Strategy” in the Development of Astronomy

Astronomy is an observational science. This paper points out that in the development of astronomy, the means of observation at every stage has as its main body the large equipment of the time, but equally important is the simultaneous development of small equipment as strategic complement. A number of historical examples are cited. The recently suggested“Special Radio Telescope Dedicated to Pulsar Research” originates in the small equipment strategy, and a brief introduction to this instrument is included here.     

Force-free magnetic fields may have a "loss of equilibrium"

By comparing the light curves in optical, hard x-ray, and soft x-ray wavelengths for 8 well-observed flares, we confirm previous results indicating that the white light flare (WLF) is associated with the flare impulsive phase. The WLF emission peaks within secondsafter the associated hard x-ray peak, and nearly two minutesbefore the 1–8 soft x-ray peak. It is further shown that the peak power in nonthermal electrons above 50 keV is typically an order of magnitudelarger, and the power in 1–8 soft x-rays radiated over 2 strdn at the time of the WLF peak is an order of magnitudesmaller, than the peak WLF power.Operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. Partial support for the National Solar Observation is provided by the USAF under a Memorandum of Undestanding with the NSF.     

"陶寺观象台"发掘与古代文献的印证

古代文献记载帝尧时的历法存在两种不同说法。羲和观测四仲中星定季节当是不实之辞,并以闰月成岁推论为使用农历也没依据。羲和观测太阳出没方位变化而"生十日"、即制订产生十月太阳历才符合事实。在文[1]中的推论,也与后一种说法可互相印证。本文对文[1]的推论作出了论据补充,与文[1]成姐妹篇。     

The Mass Function of Young Star Clusters in the "Antennae" Galaxies

We determine the mass function of young star clusters in the merging galaxies known as the "Antennae" (NGC 4038/9) from deep images taken with the Wide Field Planetary Camera 2 on the refurbished Hubble Space Telescope. This is accomplished by means of reddening-free parameters and a comparison with stellar population synthesis tracks to estimate the intrinsic luminosity and age, and hence the mass, of each cluster. We find that the mass function of the young star clusters (with ages less, similar160 Myr) is well represented by a power law of the form psi&parl0;M&parr0;~M-2 over the range 104 less, similarM less, similar106 M middle dot in circle. This result may have important implications for our understanding of the origin of globular clusters during the early phases of galactic evolution.     

火星重力场模型发展回顾及对萤火一号的展望

首先回顾了火星重力场探测的历史、各有关探测器的轨道特征和获取的资料情况,特别对最成功的MGS项目的情况作了详细介绍。然后对确定火星重力场模型过程中的有关问题作了介绍,包括动力学模型、三体摄动问题、太阳光压和大气阻力模型等。重点介绍了其中的先验条件和求解重力场的算法,后者主要介绍GSFC采用的最小二乘法和先验约束方法及其数据定权和误差校准的经验。文中还对火星重力场与地形学进行了比较分析,并对火星重力场时变性的探测与研究作了重点讨论。最后对火星重力场探测中存在的主要问题作了详细讨论,并展望了我国第一颗火星探测器"萤火一号"对火星重力场研究的可能贡献。     

An Ancient Solar Eclipse Record “Tian-da-yi“ in the 10th Century BC

The ancient record“Tian-da-yi“(the sky darkened greatly )is identified with the solar eclipse on May 31,976BC.This identification is demonstrated in this paper through a palaeographic ,astronomical and chronological analysis,It is probably the earliest solar eclipse in Chinese histroy that can be so identified.     

"水平式"施密特(Schmidt)望远镜光学系统的调整方法与步骤

近年来我们为青海德令哈观测站安装了一台施密特(Schmidt)望远镜,还把云南天文台原德制施密特望远镜机架进行了设计、改装成"水平装置".它们的改正镜口径约为Φ400mm,焦距约为800mm,用于观测人造卫星及空间碎片,用CCD作为接收器,提高了工作效率,为神州发射提供了资料.本文所述的是对这两台施密特望远镜光学系统的调整方法与步骤.