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中国计划于2025年左右建立月球轨道VLBI (Very Long Baseline Interferometer)测站,将会搭载被动型星载氢钟作为时间频率标准.由于是首次在VLBI观测中使用星载氢钟,需要研究和验证其可行性.因此,利用星载氢钟作为频率基准开展了VLBI观测.实验时,分别使用主动型地面氢钟和被动型星载氢钟作为频率基准,利用上海天文台佘山25 m射电望远镜和其他测站对我国火星探测器天问一号进行了交替VLBI观测.数据处理分析结果表明,基于地面氢钟与星载氢钟的VLBI残余群时延标准差均在0.5 ns以内,表明星载氢钟可满足深空探测VLBI测定轨的精度要求,验证了其作为月球VLBI测站频率基准的可行性. 相似文献
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在这篇文章中, 提出了一种基于改进的指数平滑和Vondrak_Cepek联合平滑的氢铯综合时间尺度产生方法. 以最小误差方法为理论基础, 动态估计氢原子钟频率漂移参数, 提升氢原子钟钟差预测准确度; 基于改进的二次指数平滑产生氢原子钟组时间尺度、加权平均方法产生铯原子钟时间尺度, 同时设计Vondrak_Cepek滤波器以结合两类时间尺度长短期稳定度优势, 提升综合时间尺度性能. 实验结果表明, 所提方法产生的氢铯综合时间尺度时稳可达1.60x10-15,天稳可达3x10-15,优于ALGOS、AT1和Kalman滤波3种经典方法产生的时间
尺度性能. 相似文献
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建立原子钟运行模型,实时预报钟差,在时频工作以及卫星导航定位中有着非常重要的意义.目前,Kalman滤波是一类重要的钟差预测模型.为了充分利用各种Kalman滤波模型的特点,提出了线性加权组合Kalman滤波模型.因此详细讨论了如何对每种Kalman滤波模型赋权,并且给出了两种简单而又实用的赋权方法.最后,以IGS(International GNSS Service)精密铷钟数据为例,运用该模型计算了预报误差.结果表明,线性加权组合Kalman滤波模型有利于提高钟差预报的准确性和可靠性. 相似文献
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氢钟和铯钟作为两种不同类型的频标,从统计角度上来说,它们在短期和长期频率稳定度方面的表现为时间频率领域中的学者们共识.随着技术的改进氢钟近年来在长稳方面有所提高.根据中国科学院国家授时中心(NTSC)新进口的2台美国氢钟(Sigma T)近一年来实验数据的分析,定量说明氢钟不同采样间隔的频率稳定度,并与铯钟的性能做比较.同时根据这两种类型频标的性能取长补短,探讨一组铯钟和两台氢钟联合守时的方案和地方原子时计算方法. 相似文献
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为提升高精度时间比对的可靠性, 结合卫星双向时间比对(Two-Way Satellite Time and Frequency Transfer, TWSTFT)和GPS精密单点定位(Precise Point Positioning, PPP)时间比对长短稳特性, 利用稳定度加权、Vondrák-\vCepek组合滤波以及 Kalman滤波融合方法对中国科学院国家授时中心(National Time Service Center, NTSC)和德国物理技术研究院(Physikalisch-Technische Bundesanstalt, PTB)间的TW-STFT和GPS PPP时间比对结果进行了融合处理并对3者进行了比较分析. 结果表明, 3种融合算法对于TWSTFT中的周日效应以及GPS PPP结果的``天跳''现象都有不同程度的改善, 融合结果与GPS PPP链路差值(Double Clock Difference, DCD)结果的绝对值保持在链路校准的不确定度范围内. 3者1d的时间和频率稳定度可以达到亚纳秒和10-15量级, Vondrák-\vCepek融合方法1d以内的稳定度最高, 适用于对短稳要求高的时间比对链路的融合. 稳定度加权、Kalman滤波融合保真度较好, 适用于对准确度要求高的时间比对链路融合. 相似文献
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守时型原子钟主要包括氢原子钟和铯原子钟,为进一步探究不同类型守时原子钟计算时间尺度相关性能,本文开展全氢钟及氢铯联合时间尺度研究。首先依据国际权度局(Bureau International des Poids et Mesures, BIPM)发布的d公报将氢原子钟进行分类,针对分类结果分别运用原子时尺度理论方法计算全氢钟时间尺度,并给出分析结果。随后计算全铯钟时间尺度,并分析探究两种不同的氢铯联合钟组时间尺度。结果表明,基于频率漂移量较小的氢钟组形成的时间尺度波动范围小,且稳定度优于频率漂移量较大的氢钟组形成的时间尺度。氢铯联合形成的时间尺度稳定度优于全铯钟时间尺度,不同的氢铯联合钟组计算得到的时间尺度结果相近。 相似文献
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地方原子时算法研究 总被引:1,自引:0,他引:1
产生和保持一个稳定、准确、可靠的时间尺度是所有时间实验室追求的目标.传统的ALGOS算法主要考虑时间尺度的长期稳定度,而地方原子时尺度需兼顾长、短期的稳定度.通过对原子钟噪声模型的分析研究,在保证地方原子时尺度长期稳定度不降低的条件下,提出适合中国科学院国家授时中心(National Time Service Center,NTSC)守时钟类型单一、钟性能相近的时间实验室计算地方时间尺度TA(NTSC)的一套完整算法.应用NTSC 2008年全年所有参加国际原子时(International Atomic Time,TAI)计算的钟的数据进行新算法的验证计算,得到的TA(NTSC)的短期稳定度指标与长期稳定度指标均有提高.研究结果适用于与NTSC守时系统结构相似的时间实验室的原子时尺度计算. 相似文献
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由单脉冲星定义的脉冲星时受几种噪声源的影响,为削弱这些影响得到一种更稳定的时间尺度,采取将多颗脉冲星定义的单脉冲星时进行综合的分析方法得到综合脉冲星时.用两种方法:经典加权算法和小波分解算法,对PSRB1855 09和PSR B1937 21两颗脉冲星进行综合计算并做出比较,经典加权算法无法兼顾脉冲星不同频率上的稳定度,而用小波分析的方法对PSR B1855 09和PSR B1937 21两颗脉冲星进行综合,能够有效抑制不同频率上噪声的影响,达到更好的效果. 相似文献
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Time synchronization between satellite and station is the key technique of satellite navigation system and the foundation of realization of satellite navigation and positioning. Aiming at solving the problems of time synchronization, we have discussed a new method of radio two-way time comparison between satellite and station, deduced in detail the reduction model of up- and down-link pseudo ranges between satellite and station, and provided a practical calculation model of clock error between satellite and station. By calculating the differences between up- and down-link pseudo ranges, this method has eliminated the influences of common errors, such as the tropospheric delay, satellite ephemeris errors, ground station coordinates errors and so on. The ionospheric delay relevant to signal frequency is also weakened largely, thus this improves the accuracy of time comparison greatly. Finally, experimental analysis is conducted by using observational data, and the results show that the accuracy of radio two-way time comparison between satellite and station can attain about 0.34 ns, which validates the correctness of theoretical method and model. 相似文献
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时间和频率技术新进展 总被引:5,自引:0,他引:5
概述了最近几年时间和频率技术的最新进展,给出了各种实用的原子频率标准的最新发展以及它们的性能指标的最新结果,介绍了国际原子时的归算方法和所达到的新水平,并对各种原子钟在归算子中的应用概况和所起的作用进行了比较,强调了氢原子钟的特殊作用和地位,同时也综述了高精度的时间同步和时频计量新技术的进展,特别是对为提高GPS这一国际时间同步辐射技术的应用水平进行的各种实验研究工作的最新进展作了进行描述,对目前 相似文献
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多任务学习方法在机器学习、计算机视觉、人工智能领域已得到广泛关注,利用任务间的相关性,将多个任务同时学习的效果优于每个任务单独学习的情况.采用多任务Lasso回归法(Multi-task Lasso Regression)用于恒星光谱物理参量的估计,不仅可以获取不同物理参量间的共同的特征信息,而且也可以很好地保留不同物理参量的特有的补充信息.使用恒星大气模拟模型合成光谱库ELODIE中的光谱数据和美国大型巡天项目Sloan发布的SDSS实测光谱数据进行实验,模型估算精度优于相关文献中的方法,特别是对重力加速度(lg g)和化学丰度([Fe/H])的估计.实验中通过改变光谱的分辨率,施加不同信噪比(SNR)的噪声,来说明模型的稳定性强.结果表明,模型精度受光谱分辨率和噪声的影响,但噪声对其影响更大,可见,多任务Lasso回归法不仅操作简便,稳定性强,而且也提高了模型的整体预测精度. 相似文献
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Mercedes T. Richards Geary E. Albright Larissa M. Bowles 《Astrophysics and Space Science》1995,224(1-2):547-548
The technique of Doppler Tomography has been used to image the accretion regions in five short-period Algols. There is clear evidence of gas flows along the predicted free-fall path of the gas stream as well as asymmetric disk-like structures around the mass gainer. Another source of H emission is associated with the cool magnetically active star. 相似文献
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Ayumi Asai Takaaki Yokoyama Masumi Shimojo Satoshi Masuda Kazunari Shibata 《Journal of Astrophysics and Astronomy》2006,27(2-3):167-173
We report a detailed examination about the relationship between the evolution of the Hα flare ribbons and the released magnetic
energy during the April 10 2001 flare. In the Hα images, several bright kernels are observed in the flare ribbons. We identified
the conjugated foot-points, by analyzing the lightcurves at each Hα kernels, and showed their connectivities during the flare.
Then, based on the magnetic reconnection model, we calculated quantitatively the released energy by using the photospheric
magnetic field strengths and separation speeds of the Hα flare ribbons. Finally, we examined the downward motions which are
observed at the Hα kernels. We found that the stronger the red-asymmetry tends to be associated with the brighter the Hα kernel. 相似文献
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We present R-band galaxy luminosity functions (GLFs) from aspectroscopic sample of six nearby rich galaxy clusters. In addition
to individual cluster GLFs, extending to, in one case, M
R=–14, we also present composite GLFs for cluster and field galaxies toM
R=–17. All six cluster samples are consistent with the composite GLF, but there is evidence that the GLF of the quiescent population
in clusters is not universal. Furthermore, the GLF of quiescent galaxies is significantly steeper in clusters than in the
field. The overall GLF in clusters is consistent with that of field galaxies, except for the luminous tip, which is enhanced
in clusters versus the field.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
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K. G. Strassmeier R. Pallavicini J. B. Rice M. I. Andersen F. M. Zerbi 《Astronomische Nachrichten》2004,325(4):278-298
We lay out the scientific rationale for and present the instrumental requirements of a high‐resolution adaptiveoptics Echelle spectrograph with two full‐Stokes polarimeters for the Large Binocular Telescope (LBT) in Arizona. Magnetic processes just like those seen on the Sun and in the space environment of the Earth are now well recognized in many astrophysical areas. The application to other stars opened up a new field of research that became widely known as the solarstellar connection. Late‐type stars with convective envelopes are all affected by magnetic processes which give rise to a rich variety of phenomena on their surface and are largely responsible for the heating of their outer atmospheres. Magnetic fields are likely to play a crucial role in the accretion process of T‐Tauri stars as well as in the acceleration and collimation of jet‐like flows in young stellar objects (YSOs). Another area is the physics of active galactic nucleii (AGNs) , where the magnetic activity of the accreting black hole is now believed to be responsible for most of the behavior of these objects, including their X‐ray spectrum, their notoriously dramatic variability, and the powerful relativistic jets they produce. Another is the physics of the central engines of cosmic gamma‐ray bursts, the most powerful explosions in the universe, for which the extreme apparent energy release are explained through the collimation of the released energy by magnetic fields. Virtually all the physics of magnetic fields exploited in astrophysics is somehow linked to our understanding of the Sun's and the star's magnetic fields. (© 2004 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献