对地方电视台转播CCTV时延的测定

讲述了同步广播卫星电视时间信号的测量方法和测量结果，获得了CCTV1、CCTV2通过同一颗卫星（亚太－1A）转播的时延差值为16333μs，测量精度在10ns以内；CCTV2、CCTV4分别经两颗卫星（亚太－1A、亚洲－Ⅱ）转播，在陕西天文台卫星地面接收站时延差值为1644．20μs，精度为50μs，并分析了影响时延差值和精度的原因。同时测量了地方电视台转播亚太－1A的CCTV信号与直接接收亚太－1A的CCTV信号的时延差值，其测量精度为0．1μs。这些结果为利用同步广播卫星的电视信号进行高精度的时间服务提供了参考依据。     

关中平原大地等效电导率的间接测量

为准确预报地波传播时延,用电波传播法对关中平原的大地等效电导率进行了间接测量。阐述了电波传播法的测量原理和方法,第一次给出关中平原大地等效电导率的间接测量结果,同时,给出了中国科学院国家授时中心临潼科研楼参考点的BPL信号传播时延测量结果,并对这些测量结果进行了精度分析。     

对地方电视台转播CCTV时延的测定

讲述了同步广播卫星电视时间信号的测量方法和测量结果，获得了ＣＣＴＶ、ＣＣＴＶ２通过同一颗卫星（亚太－１Ａ）转播的时延差值为１６３．３３μｓ，测量精度在１０ｎｓ以内；ＣＣＴＶ２、ＣＣＴＶ４分别经两颗卫星（亚太－１Ａ，亚洲－Ⅱ）转播，在陕西天文台卫星地面接收站时延差值为１６４４．２０μｓ，严谨为５０μｓ，并分析了影响时延差值和精度的原因，同时测量了地方电视台转播亚太－１Ａ的ＣＣＴＶ信号与直接接收亚太－     

电磁波在太阳引力场中传播速度的变化对VLBI时延测量的影响

太阳引力场效应对高精度VLBI时延测量有较大影响。本比较了两种改正太阳引力场效应的计算方法－－基于太阳引力偏折的方法和较差光行时方法，并由此得到结论：引力偏折与较差光行时是两个不同的概念；它们两对VLBI时延测量的影响的量级相同，但相差一个主项，即引力场中电磁波速度大小的变化引起的附中时延；另外二还相差一些小项。     

无线电长波传播时延的测量

为了在长波授时与导航系统中,进行传播时延的修正,研究电波传播时延修正的理论及方法,及通过传播时延的测量测定土地等效导电率等,必须对电波传播的时延进行精确的测量。利用飞机搬运原子钟方法就是一种高精度的测量长波传播时延的方法。一九七八年十月至十一月进行的3262工程电波传播搬运钟试验,采用飞机搬运铷原子钟测量了我国不同传播路径上许多地点长波天、地波传播的时延,测量的精度为±0.14μs。下面我们就这次实验中传播时延的测量问题进行分析讨论。     

基于UTC（NTSC）的GPS定时接收机时延测量

GPS提供了一种精密定时的方法,但接收机绝对时延的测量是一个难题,现有的测量方法成本高且难以操作,因而提出了一种GPS定时接收机时延测量的简单方法。这种方法根据国家授时中心保持的时间尺度UTC（NTSC）与GPS定时接收机输出的秒脉冲信号（1PPS）的比对结果,利用UTC（NTSC）的国际比对数据以及UTC与GPST的时差数据,可以测量GPS定时接收机时延,该方法简单易行。最后,对这种方法的测量误差进行了分析。     

微波时间传递精度和时延分析

分析了引起微波时间传递系统时延变化的原因和单向及双向时间传递比对精度;分析表明,根据微波双向时间比对的长期测量数据可对搬钟实验得到的时延值进行修正,采用该修正结果可减小单向时间比对的误差。     

CygX—1硬态高能光子的时延

硬X射线和软射线光子的时延时研究主能辐射的一个重要方面，傅里叶交叉谱常常被用于教育处硬软光子之间的时延，但是交叉说示能在高于30Hz的傅里叶频率上从CygX-1测量到有统计意义的快速光变，由李惕培在时域上发展的交叉相关函方法能有效测量不同时间尺度上的时延，利用此交叉相关分析方法，讨论了不同观测时期CygX-1硬态高能光子时延 的性质，分析结果表明，CygX-1硬态在短的尺度（＜0．1秒）上存存在有意义的时间延迟，并将短时间尺度上的观测结果和各种CygX-1硬态模型进行了比较讨论。     

基于天文开源软件的卫星干涉测量数据处理系统

VLBI (Very Long Baseline Interferometry)技术观测卫星需要对干涉测量数据进行相关和后处理,通过相关、时延校准、条纹搜索,最终得到卫星的基线几何时延.基于天文开源软件建立起一套卫星干涉测量数据处理系统.该系统可工作在实时和事后两种状态,实现相关、中性大气、电离层、钟模型以及仪器硬件的时延校准、条纹搜索、生成基线时延和时延率序列.使用该系统处理北斗GEO (Geosynchronous Earth Orbit)卫星的干涉测量试验数据,得到了精度在1–2 ns量级的卫星基线时延序列.     

探月卫星同波束VLBI差分相位时延闭合计算与分析

针对同波束干涉测量中差分相位时延模型验证、解算结果周跳检测与校正问题进行分析。给出了相位闭合和差分相位时延闭合计算原理与方法,并以SELENE任务中解算的差分相位时延数据为算例进行分析,差分相位时延闭合计算结果小于几皮秒。验证了差分相位时延基于同一波前的模型,可用于对差分相位时延中周跳问题进行检测,可对数据波动情况进行监视,为数据后处理提供依据。在实际应用中,该方法可随着数据处理过程的推进同步进行,因此,十分有利于同波束干涉测量方法的实时实施,并应用于卫星导航。     

GPS共视中电离层时延计算方法比较研究

为了更好地计算GPS CV（共视）时间传递中的电离层时延值（它是影响CPS CV比对结果精度的主要因素之一）,介绍了当前3种电离层时延的计算方法,并以NICT（National Institute of Information and Communications Technology）单站GPS比对数据及NICT与NTSC（National Time Service Center）的GPS共视比对数据为例,分析比较了不同的电离层时延计算方法对GPS时间比对结果精度的影响。计算结果表明：利用双频实测电离层时延和利用ICS（International GPS Service）提供的TEC（total electton content）map计算的电离层时延对GPS CV比对结果修正后的精度,比利用电离层改正模型的时延对比对结果修正后的精度分别提高30％～40％和20％～30％。     

When is star formation episodic? A delay differential equation 'negative feedback' model

We introduce a differential equation for star formation in galaxies that incorporates negative feedback with a delay. When the feedback is instantaneous, solutions approach a self-limiting equilibrium state. When there is a delay, even though the feedback is negative, the solutions can exhibit cyclic and episodic solutions. We find that periodic or episodic star formation only occurs when two conditions are satisfied. First the delay time-scale must exceed a cloud consumption time-scale. Secondly, the feedback must be strong. This statement is quantitatively equivalent to requiring that the time-scale to approach equilibrium be greater than approximately twice the cloud consumption time-scale. The period of oscillations predicted is approximately four times the delay time-scale. The amplitude of the oscillations increases with both feedback strength and delay time.
We discuss applications of the delay differential equation (DDE) model to star formation in galaxies using the cloud density as a variable. The DDE model is most applicable to systems that recycle gas and only slowly remove gas from the system. We propose likely delay mechanisms based on the requirement that the delay time is related to the observationally estimated time between episodic events. The proposed delay time-scale accounting for episodic star formation in galaxy centres on periods similar to   P ∼ 10 Myr  , irregular galaxies with   P ∼ 100 Myr  , and the Milky Way disc with   P ∼ 2  Gyr, could be that for exciting turbulence following creation of massive stars, that for gas pushed into the halo to return and interact with the disc and that for spiral density wave evolution, respectively.     

脉宽调制(PDM)发射机时延的分析测量

在对我国BPM短波授时台目前使用的脉宽调制（PDM）发射机的电路结构,时频特性,调制信号失真及影响时延变化的因素作分析的基础上,对脉宽调制（PDM）发射机时延进行了分析测量,这一工作不但为授时发播控制提供了参考,还有助于时频工作对这种发射机有关时频性能的了解。     

Orbit determination of satellite “Tance 1” with VLBI data

The satellite “Tance 1” of the “Double-Star Program” is the first truly scientific experimentation satellite of China. Its orbit is the farthest so far launched in China, with a geocentric apogee reaching 78 thousand kilometers. The tracking of “Tance 1” and of more distant space targets, such as the lunar exploration craft, can be realized with the VLBI technique of radio astronomy. In order to test and verify the role which the VLBI technique plays in the lunar exploration program of China, Shanghai Astronomical Observatory organized the only 3 tracking stations in China (located at Shanghai, Urumqi and Kunming), to carry out test tracking of “Tance 1,” and used the time delay data obtained to determine the orbit of “Tance 1” over a two-day period, so providing a preliminary assessment of the possibility of VLBI orbit determination. The fitting error of the orbit so obtained is about 5.5 m in the time delay and about 2 cm/s in the delay rate (this for checking only), much better than is provided by the preliminary orbit (used merely for ensuring tracking) in which the corresponding figures are around 2 km and 15 cm/s. Further, if the orbit is determined by using both the time delay and time delay rate data (with weights according to their internal accuracies), then the residuals are 5.5 m in the time delay and 2 cm/s in the delay rate. For an appreciation of the true accuracy of the VLBI orbit determination, we used simulation data (of the observed two-day VLBI data) and found the results depended greatly on the error in the dynamic model of the satellite which, however, is difficult to assess, while the formal residuals are of the order of 1 kin in the delay and of cm/s in the delay rate. The simulation computation also indicates that a joint determination using both VLBI and USB data will have an improved accuracy.     

GPS共视时间比对中的电离层时延改正问题

众所周知，GPS共视是目前国际上主要的时间传递比对技术，其中扣除电离层时延是很重要的一个方面。介绍了如何采用国际GPS服务中心(IGS-International GPS Service)公布的电离总电子含量(TEC-Total Electron Content)图来进行电离层时延改正。结果表明：对于单频GPS接收机，采用TEC图作电离层时延改正后的单站定时和共视比对精度比用理论模型作改正的精度有很大的提高。通过比较还表明，亚太地区的时间实验室之室的时间传递精度比欧美地区的要低，这可能是因为亚太地区用于测量TEC的IGS测站少，因而导致该地区的TEC的精度较低。     

A model of geometric delay in Space VLBI

A model which includes the relativistic effect is derived that can be applied to space very long baseline interferometry(SVLBI) while taking observations of sources at infinite distance. In SVLBI,where one station is on a spacecraft,the length of the baseline and the orbiting station's maximum speed in an elliptical orbit around the Earth is much larger than the ground-based VLBI,which leads to a larger delay and higher delay rate. The delay models inside VLBI correlators are usually expressed as fifth-order polynomials during a limited time interval,which are evaluated by firmware in the correlator and track delays in the interferometer over the limited time interval. The higher SVLBI delay rate requires more accurate polynomial fitting and evaluation,as well as more frequent model updates.     

Effect of magnetic activity on ionospheric time delay at low latitude

The purpose of this work is to investigate the effect of magnetic activity on ionospheric time delay at low latitude Station Bhopal (geom. lat. 23.2°N, geom. long. 77.6°E) using dual frequency (1575.42 and 1227.60 MHz) GPS measurements. Data from GSV4004A GPS Ionospheric Scintillation and TEC monitor (GISTM) have been chosen to study these effects. This paper presents the results of ionospheric time delay during quiet and disturbed days for the year 2005. Results show that maximum delay is observed during quiet days in equinoxial month while the delays of disturbed period are observed during the months of winter. We also study the ionospheric time delay during magnetic storm conditions for the same period. Results do not show any clear relationship either with the magnitude of the geomagnetic storm or with the main phase onset (MPO) of the storm. But most of the maximum ionospheric time delay variations are observed before the main phase onset (MPO) or sudden storm commencement (SSC) as compared to storm days.     

Constraints on Extra-Dimensions and Variable Constants from Cosmological Gamma-Ray Bursts

The observation of the time delay between the soft emission and the high-energy radiation from cosmological gamma ray bursts can be used as an important observational test of multi-dimensional physical theories. The main source of the time delay is the variation of the electromagnetic coupling, due to dimensional reduction, which induces an energy dependence of the speed of light. For photons with energies around 1 TeV, the time delay could range from a few seconds in the case of Kaluza–Klein models to a few days for models with large extra-dimensions. Based on these results we suggest that the detection of the 18-GeV photon ∼4500 s after the keV/MeV burst in GRB 940217 provides a strong evidence for the existence of extra-dimensions. The time delay of photons, if observed by the next generation of high energy detectors, like, for example, the SWIFT and GLAST satellite based detectors, or the VERITAS ground-based TeV gamma-ray instrument, could differentiate between the different models with extra-dimensions.