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电磁兼容性是设备或系统的重要性能指标, 也是保障系统的工作效能和提高系统可靠性的重要因素. 大口径射电望远镜运行阶段, 台址周围无线电业务及内部潜在的电磁干扰会降低观测系统灵敏度、影响天文观测的质量. 本论文针对拟建的新疆110 m全向可动射电望远镜(Qi Tai raido Telescope, QTT)开展了系统电磁兼容评估技术及控制方法研究, 具有重要的工程应用价值. 首先, 依据现有电波环境测量方法的不足, 深入分析了仪器设备的关键参数配置方法及测量时间计算方法, 采用Y因子法校准测量数据, 提出一种准实时电波环境测量方法. 面向高重复性宽带频谱, 分析了宽带频谱信号和噪声特征, 结合标准差理论, 提出一种基于邻值比较的信噪分离方法, 并采用邻值统计方法优化关键参数, 提高信噪分离精度. 针对QTT台址, 开发了自动化电波环境监测系统, 该系统6 GHz以下频段系统增益大于40 dB, 系统噪声系数小于2 dB, 测量不确定度小于1.49 dB, 具有极高的系统灵敏度和测量精度; 分析了频谱监测数据流, 设计了基于HDF5 (Hierarchical Data Format version 5)的数据存储格式, 开发了自动化电波环境测量和监控软件及数据处理软件. 依据QTT台址长期监测数据, 评估分析了台址电磁环境、主要干扰源特征及其影响. 其次, 提出大口径射电望远镜馈源口面干扰电平限值量化方法, 建立了基于台址地形的电波传播模型, 分析了现有电波传播模型的优缺点及适应性, 结合QTT台址实际地形及地质特征, 采用Longley-Rice和Two-Ray电波传播模型, 预测分析了QTT台址潜在干扰区域电磁干扰达到射电望远镜的电波路径衰减, 结合大口径射电望远镜天线增益量化方法, 提出设备所在位置干扰电平限值量化方法, 运用该方法对QTT台址潜在干扰区域的干扰电平限值进行量化. 依据设备所在位置干扰电平限值, 调研分析了国内外军用、民用电磁兼容测量标准, 结合电磁干扰对射电天文观测的影响, 提出一种大口径射电望远镜电磁兼容控制方法, 解决了现有电波暗室测量系统无法直接测量评估电子设备电磁兼容的问题, 该电磁兼容控制方法计划应用于QTT建设及运行阶段, 确保系统拥有良好的电磁兼容性. 最后, 依据QTT台址潜在干扰区域干扰电平限值, 结合典型电子设备电磁辐射频谱, 分析了QTT电磁兼容设计需求, 提出电磁兼容设计初步方案. 另外, 针对台址建筑设施内的中低电磁辐射干扰源, 提出一种低成本建筑屏蔽方法, 应用于QTT台址现有建筑. 相似文献
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本文分析了地球自转角速度的变化对脉冲星的周期变率P的影响,得出以下结果:(1)地球自转角速度的变化对每一脉冲星的脉冲周期和周期变率都存在影响,因此,在把地球上所测量的脉冲星脉冲到达时间归算到太阳系质心时,必须考虑地球自转角速度变化的影响。(2)地球自转角速度的变化对脉冲星的周期影响不大,但对周期变率的影响必须引起注意,特别是对于P较小的脉冲星,这种影响甚至可大于本体的周期变化。(3)地球自转角速度的变化对脉冲星周期变率影响的数值,取决于脉冲星的赤纬和观测台站的纬度;赤纬越大,纬度越高,其值越小。(4)在上、下中天观测,地球自转角速度的变化对脉冲星的周期变率的影响较大。 相似文献
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用球谐函数方法（SHM）计算了由Schwiderski海潮图和日本海海潮图引起的M2,S2,K1和O1各分潮波的综合海潮负荷参数.计算中采用了Pagiatakis（1990）地球模型的负荷Love数.结果表明SHM具有更高的计算效率和计算精度．为了真正实现±毫米的VLBI地壳运动测定精度和±0.1微伽的绝对重力测量精度,对未来海潮图模型,特别是日本海的海潮图模型的精度要求作了讨论．计算结果还表明不同地球模型的负荷Love数对计算的测站位移之差为0.7毫米,在目前测量精度下尚可以不作考虑.中国近海的海潮M2波对台北,上海,Daejeon,Okinawa,和Kagosima站的径向和水平分量位移影响可分别达±22．4～±1．0毫米和±05-±5.5毫米,表明中国近海高精度的海潮图模型对东亚测站的地壳运动高精度测量是十分重要的． 相似文献
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全球动力学扁率(H)是研究地球自转与岁差的-个重要物理量.由对岁差的观测有Hobs=0.0032737≈1/305.5.该文依据内部场理论重新计算了流体静平衡态下的地球内部几何扁率剖面,结果与Denis(1989)的结果相吻合.该文还推导了三阶扁率精度下日的计算式,并计算出PREM地球模型的H理论值为HPREM=1/308.5,这与其他人的结果一样,与观测值之间存在1%的差别.为了研究这个差别的来源,该文将PREM模型中均一的上地壳层与海洋层替换为ECCO、GTOPO30和ETOPO5等真实的地球表层数据,结果表明替换后得到的H更加偏离观测值.此结果说明来自于地幔及更深处质量异常引起的正面影响可能要比先前预期的高,并为地壳均衡理论提供了间接的证据. 相似文献
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王广利 《中国科学院上海天文台年刊》1996,(17):80-88
根据1989年到1994年期间MKⅢ的测地VLBI观测资料，对总共423次实验的26973个延迟测量值作了分析处理，得到了站的台站坐标、运动速度、基线长度和基线长度变化率以及射电源位置的测量结果。 相似文献
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《天文学报》2016,(6)
使用紫金山天文台盱眙观测站近地天体望远镜对WASP-43 b和TrES-3 b分别做了2次和4次凌星主食的测光后续观测.经过较差测光和光变曲线拟合,分别得到了两个系统的相关物理参数,结果与之前的文献结果吻合.结合多篇文献中的数据,对两个系统凌星中心时刻的观测残差O-C分别作了线性和二次函数拟合,根据线性拟合得到了行星的轨道周期及凌星中心时刻变化即TTV,分析后认为在两个系统中尚未发现明显的周期性TTV信号,并给出了WASP-43和TrES-3系统中1:2轨道共振位置上可能存在行星的质量上限分别为1.826和1.504个地球质量.通过二次函数拟合,尚未发现TrES-3b存在长期TTV即轨道衰变;证认了WASP-43 b可能存在轨道衰变,得到其轨道衰变率P=(-0.005248±0.001714)s·yr~(-1),并与文献中的相关结果做了比较,还据此计算出了该系统的恒星潮汐质量参数下限为Q_*~'≥1.5×10~5,并分别对两个系统中不同的Q_*~'值给出了相应的行星剩余寿命. 相似文献
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基于NNR-NUVEL-1A地球板块运动模型和ITRF2000地球参考架的三维VLBI站速度矢量,采用实测的VLBI基线长度变化率作为约束,重新估计了部分国际VLBI站的局部或区域性地壳的垂直形变,并与国际地球参考架ITRFs解和VLBI全球解GLB2003,VTRF2003和VTRF2005的结果进行了比较。结果表明,欧亚板块的URUMQI站和太平洋板块的KWAJAL26站,南极OHIGGINS站的垂直形变率、ITRFs解和VLBI全球解存在6-15mm/a的差异,北美YUMA站可能有15-31mm/a 的垂直形变率,而美国西部太平洋板块的San Francisco(PRESIDIO)站的垂直形变率还有待进一步的研究。此外,SC-VLBA,CRIMEA和EFLSBERG站的垂直形变率、ITRFs解和VLBI全球解的差约为1-6mm/a。用不同方法得到的VLBI站的水平形变率解有较好的一致性。 相似文献
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全球导航卫星系统(Global Navigation Satellite System,GNSS)接收机在接收卫星信号后,经过捕获、跟踪,得到码相位与载波相位两个基本测量值,然后通过测量值计算卫星与接收机之间的距离.载波相位测量值比码相位测量值具有更高的测量精度,但由于载波相位测量值具有计算整周模糊度的问题,得到高精度... 相似文献
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Abstract— Meteorite magnetic records constitute physical evidence of processes acting during early solar system evolution. Consequently, the validation of these records is important in meteorite research. The first step in the validation process should be the REM value. The REM value is the ratio of natural remanence (NRM) to saturation remanent magnetization imparted by a 1 T magnetic field (SIRM). The REM values range over 3 to 4 orders of magnitude for stony meteorites and for chondrules from Allende (C3V‐S1), Bjurböle (L4‐S1), and Chainpur (LL3‐S1) meteorites. The REM values computed from published NRM and SIRM data identify many orders of magnitude range in the REM values including REM values >100 × 10?3. These data suggest a dependence for the NRM intensity on the curatorial location from which the sample was obtained. Any earth rock acquiring thermoremanent magnetization (TRM) in the geomagnetic field has a restricted range in REM mostly between 5 and 50 × 10?3, the exception being the mineral hematite in the multidomain size range. The only terrestrial samples with REM much greater than 100 × 10?3 are those struck by lightning. The REM value provides a physical basis for recognition between valid records and those that “might be contaminated.” The isothermal remanence acquisition (RA) curve is presented as a contamination curve that allows an indication of the level of magnetic field contamination required to give the computed “REM” (RM/SIRM) value. In the case of the Bjurböle and Chainpur chondrules, with REM values >100 × 10?3, the RA curve indicates that unrealistically large contamination magnetic fields would be required to give REM values greater than 100 × 10?3. This would suggest contamination other than by a hand magnet that is normally available to an experimenter. This would require an explanation that would involve large magnetic fields during chondrule formation, or some extraordinary remanence acquisition mechanism that remains to be described. Magnetic contamination experiments, using ～80 and ～40 mT magnets, demonstrate that the “REM” values and extent of modification of the magnetic vector record are mineralogy dependent, and this is mostly related to the amount and characteristics of the mineral tetrataenite. The complexity of the meteorite records suggest validation of the record as a first step. The REM value is the first physical statement that can be made in this validation. 相似文献
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The very-low-frequency emission known as “chorus” has been studied for four Australian recording stations. The phenomenon exhibits a maximum of occurrence at about geomagnetic latitude 60° and occurs only about one-tenth as frequently at geomagnetic latitude 45°. It was never definitely observed at geomagnetic latitude 35°. Marked diurnal variations are present with morning peaks for all stations and also an evening peak at Adelaide and Hobart. Analysis of the diurnal variations suggests that two different mechanisms are involved. The average strength of chorus increases with increasing value of K-index at lower latitude stations and shows a maximum at moderate values of the index for geomagnetic latitude 61°. This is interpreted as meaning that the region of maximum average-chorus-strength moves towards lower latitudes at times of magnetic disturbance. 相似文献
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The mean photospheric magnetic field of the sun seen as a star has been compared with the interplanetary magnetic field observed with spacecraft near the earth. Each change in polarity of the mean solar field is followed about 4 1/2 days later by a change in polarity of the interplanetary field (sector boundary). The scaling of the field magnitude from sun to near earth is within a factor of two of the theoretical value, indicating that large areas on the sun have the same predominant polarity as that of the interplanetary sector pattern. An independent determination of the zero level of the solar magnetograph has yielded a value of 0.1±0.05 G. An effect attributed to a delay of approximately one solar rotation between the appearance of a new photospheric magnetic feature and the resulting change in the interplanetary field is observed. 相似文献
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介绍了国际测地/天体测量学甚长基线干涉测量服务(International Very Long Baseline Interferometry (VLBI) Service for Geodesy and Astrometry, IVS)组织机构及下属分析中心概况.系统归纳了目前IVS发布的地球定向参数(Earth Orientation Parameters, EOP)产品类型及不同观测类型的用途.利用2010—2019年公开发布的观测资料,对IVS不同分析中心的EOP日常监测和服务能力进行了评估.通过构造观测台站所构成的几何体积,分析了EOP精度与测站数量、测站网分布的关系,统计了IVS不同观测类型的EOP解算精度.此外,综合公开发布的美国、欧洲等区域网观测数据,分析了不同地区区域网的常规及加强观测结果与IVS结果的差异.结果表明:EOP的解算精度与观测台站的分布密切相关, IVS常规观测确定的极移分量的外符合精度优于0.2 mas,世界时(Universal Time, UT1)与协调世界时(Coordinated Universal Time,UTC)之差(UT1-UTC)的精度在0.015 ms左右,加强观测的UT1-UTC值与国际自转服务组织(International Earth Rotation Service, IERS)的C04之间存在0.02–0.03 ms的差异.区域观测网的精度受观测网形和基线长度制约,总体劣于IVS观测精度,其中,美国甚长基线干涉阵列(Very Long Baseline Array, VLBA)的常规及加强观测结果与IVS全球观测结果最接近. 相似文献
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COSMIC计划 总被引：10，自引：0，他引：10
为了获得足够多的地面掩星点资料，用于全球和局部天气预报和大气研究，1997年中国台湾地区和美国联合制定了耗资1亿美元的COSMIC（Constellation Observing System for Meteorology，Ionosphere and Climate)计划。COSMIC是气象、电离层和气候星座观测系统，它包括卫星、地面数据接受和卫星控制站、数据分析中心和数字通讯网络，计划于2005年开始实施。介绍了COSMIC计划产出的历史背景、科学任务及其整个系统的组成，并针对COSMIC和其它LEO（低地球轨道）星座计划，提出了我们应做和正在做的研究工作。 相似文献
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利用中国地壳运动观测网络1999～2006年的观测数据,计算出川滇地块及其邻区内中国地壳运动观测网络中151个监测站在欧亚参考框架下的水平速度,水平运动速度大小在3.44～19.74 mm/a之间,平均为11.68 mm/a。分析川滇地块及其邻区内测站运动方向的变化得出:川滇地块及其邻区在围绕喜马拉雅东结点作顺时针旋转,川滇地块南北方向上存在明显的挤压,东西方向上存在延伸现象。使用最小二乘法求得川滇地块整体运动速度的大小为13.36 mm/a,运动方向为东偏南64.9°,川西北次级块体的运动速度的大小为15.66mm/a,运动的方向为东偏南52.1°。滇中次级块体的运动速度的大小为12.57 mm/a,运动方向为东偏南72.4°。 相似文献
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A magnetospheric boundary and its associated standing-shock wave for the earth are scaled down in size to apply to Mars. A suggestion by the Mariner-IV experimenters that their magnetometer may have detected a Martian shock at 0123 UT (earth) on July 15, 1965, is accepted. The scaling procedure used previously in the case of the Mariner-II flyby of Venus on December 14, 1962, as well as in the present case of Mars is repeated but with a different model. We propose a magnetospheric boundary for the earth, which is based on a maximum radius of 22 R
E suggested by Imp-1 magnetometer data. We further suggest a low value (1.2) of the adiabatic exponent, . In addition we propose the use of the interplanetary magnetoacoustic Mach number, M*, which is a combination of both Alfvén and ordinary gasdynamic Mach numbers. Our choice of values for these parameters is not unique since many such combinations exist which will show good agreement with observation. For example, the ratio of the Martian dipole moment to that for the earth is found to be 2.1 × 10–4 by our application of the hypersonic analog. This value compares very closely with 3 × 10–4 deduced as an upper bound by the Mariner-IV investigators. The present synthesis is presented as an independent calculation based on the above theoretical considerations, together with the experimenters' probable observation of a Martian shock wave.Since this paper was submitted for publication, theoretical calculations of the steady-state average magnetic induction in the transition region for an interplanetary field oriented at several angles to the velocity vector have been published by A. Y. Alksne, Planetary Space Science
15 (1967), 239–245. As anticipated in the text above, the magnitudes are slightly changed, but the polarities are significantly different.Formerly the Central Radio Propagation Laboratory of the National Bureau of Standards. 相似文献
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在卫星电视授时系统方案中，为确定标准秒信号从发射站经卫星到用户接收站的传播时延值，需要知道收、发地面站及卫星的坐标，所以，在高精度的卫星电视授时系统中，需要建立高精度的同步卫星定位同。本文提出在没有卫星定位同的条件下，用非坐标方法来确定卫星时间信号到用户的传递时延，其授时精度为几μｓ。 相似文献
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Leonid S. Lyubimkov Tamara M. Rachkovskaya Sergey I. Rostopchin David L. Lambert 《Monthly notices of the Royal Astronomical Society》2002,333(1):9-26
Effective temperatures T eff , surface gravities log g and interstellar extinctions A V are found for 107 B stars. Distances d of the stars, which are based on the derived T eff , log g and A V values, show good agreement with those obtained from the Hipparcos parallaxes. Comparing the T eff and log g values with evolutionary computations, we infer masses, radii, luminosities, ages and relative ages of the stars. Empirical relations between the T eff and log g parameters, on the one hand, and the photometric indices Q , [ c 1 ] and β , on the other hand, are constructed; these relations give a fast method for the T eff and log g estimation of early and medium B stars. Inclusion of the infrared J , H and K colours into the T eff , log g and A V determination shows that (i) the T eff and log g parameters are altered only slightly; (ii) the A V value is rather sensitive to these colours, so an accuracy better than 0.05 mag in the JHK data is necessary for precise A V evaluation. 相似文献