共查询到20条相似文献，搜索用时 156 毫秒
1.
XIA Haibo 《中国科学院上海天文台年刊》2004,(1)
Daubechies小波可以表征为幂函数或e指数函数的形式 ,保持相关相位条纹的幅角不变。在VLBI观测信号相关处理过程中引入了小波分析方法 ,以探讨小波理论在VLBI技术中的应用特点。两个台站的VLBI观测信号经过时间补偿和干涉条纹旋转后 ,利用静态小波算法在线性空间中的保角变换特征可提取VLBI信号的干涉相位特征 ,并完整保留相位的时序关系。 相似文献
2.
夏海波 《中国科学院上海天文台年刊》2004,(25):69-73
Daubechies小波可以表征为幂函数或e指数函数的形式，保持相关相位条纹的幅角不变。在VLBI观测信号相关处理过程中引入了小波分析方法，以探讨小波理论在VLBI技术中的应用特点。两个台站的VLBI观测信号经过时间补偿和干涉条纹旋转后，利用静态小波算法在线性空间中的保角变换特征可提取VLBI信号的干涉相位特征，并完整保留相位的时序关系。 相似文献
3.
在射电天文观测中,射频干扰(Radio Frequency Interference, RFI)会以多种形式混入望远镜接收系统,给观测带来误判或者降低观测信噪比.近年来国内国际射电天文快速发展,国内国际大型射电望远镜和阵列先后建设,观测灵敏度大为提高,射频干扰的影响尤为突出.随着科技发展和人类活动的加剧,射频干扰日益严重且不可逆转.提出利用2维离散小波变换的方法分析射电天文观测的数据,对望远镜系统输出的时间频率序列进行小波变换,根据小波系数分离出原始信号中各分量,每个分量统计得到相应的阈值,将各分量与阈值相比较识别干扰成分并标记去除.利用该方法对实际观测数据进行了处理,结果表明该方法能够很好地标记并消减干扰信号,且提高了观测的信噪比. 相似文献
4.
5.
蒋世仰 《中国天文和天体物理学报》1983,(3)
本文从实际天文课题出发,定量地分析了 Fellgett增益和Jacquinot增益。指出只有在接收器噪音远大于光子噪音及其它噪音的某些红外区,以及在其它波段打算用视场很大的中小望远镜或干脆不用望远镜直接观测角直径很大的广谱天体的总体光谱的精细结构时,傅里叶变换分光仪才真正优于光栅分光仪。 相似文献
6.
在GPS数据处理中 ,存在着误差影响、影响波的干扰、周跳和数据量大等问题。误差影响和影响波的干扰实质是在接收卫星信号时受到其它因素的影响 ;周跳是由于卫星信号的失锁而造成信号的不连续 ;数据量大是因为GPS观测需要采样间隔小又连续观测所致。由于小波理论具有时频分析、波形分解、特征提取和快速小波变换等特性 ,应用小波变换和波形分解可以解决误差影响和影响波的干扰的问题 ;应用特征提取可以解决周跳检测问题 ;应用快速小波变换可进行数据压缩 相似文献
7.
用２。１６ｍ望远镜及其卡焦光谱仪对Ｎｏｖａ Ｏｐｈ １９９４进行了一系列的光谱观测，其早期光谱中出现的大量Ｆｅｌｌ线表明它是一颗Ｆｅｌｌ型新星，而它的发射线的多峰结构在其它Ｆｅｌｌ型新星中是不多见的，它们根据得到的光谱和从国际互联网络得的测光资料，讨论了它的光谱特征和演化。 相似文献
8.
小波分析理论在GPS技术中的应用 总被引：6，自引：0，他引：6
在GPS数据处理中，存在着误差影响、影响波的干扰、周跳和数据量大等问题。误差影响和影响波的干扰实质是在接收卫星信号时受到其它因素的影响；周跳是由于卫星信号的失锁而造成信号的不连续；数据量大是因为GPS观测需要采样间隔小又连续观测所致。由于小波理论具有时频分析、波形分解、特征提取和快速小波变换等特性，应用小波变换和波形分解可以解决误差影响和影响波的干扰的问题；应用特征提取可以解决周跳检测问题；应用快速小波变换可进行数据压缩。 相似文献
9.
用２．１６ｍ望远镜及其卡焦光谱仪对ＮｏｖａＯｐｈ１９９４进行了一系列的光谱观测，其早期光谱中出现的大量ＦｅＩＩ线表明它是一颗ＦｅＩ型新星，而它的发射线的多峰结构在其他ＦｅＩＩ型新星中是不多见的．我们根据得到的光谱和从国际互联网络（Ｉｎｔｅｒｎｅｔ）得到的测光资料，讨论了它的光谱特征和演化． 相似文献
10.
分析ＲＸＴＥ卫星ＰＣＡ探测器对ＣｙｇＸ－１的观测数据,得到了其处于高态及高低高转换时的Ｘ射线短时标爆发（Ｓｈｏｔ）结构。在所观测到的三种态中是不对称的,并且不同的状态中Ｓｈｏｔ的结构有明显差异。Ｓｈｏｔ前后沿可分别由双指数函数近似拟合。Ｓｈｏｔ中的快时变过程是由慢的上升前沿和快的下降后沿构成。在所观测态中Ｓｈｏｔ平均宽度约为０．１１秒（ＦＷＨＭ）,比低态时的宽度窄。同一状态中高能段的Ｓｈｏｔ宽度较 相似文献
11.
H.J. Haubold 《Astrophysics and Space Science》1997,258(1-2):201-218
Wavelet analysis offers an alternative to Fourier based time- series analysis and is particularly useful when spectral features
are time dependent. We analyze the solar neutrino capture rate of the radiochemical Homestake chlorine experiment with abbreviated
Morlet wavelets, using Foster's (AJ, 111,1709(1996)) rescaled wavelet technique. We emphasize the complementarity of wavelet
analysis to Fourier analysis. Wavelet analysis confirms the results of previously undertaken Fourier analysis. The Homestake
data seem to contain a harmonic content with periodicities of 4.76 yr, 1.89 yr, 0.85 yr, and 0.51 yr. Wavelet analysis reveals
that the 4.76 yr and 1.89 yr periods show an almost constant behavior over the 25 yr Homestake data record, while the 0.85
yr and 0.51 yr periods exhibit a transient phenomenon. The analysis does not show strong evidence for a period of the solar
11 yr cycle.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
12.
Wavelet Analysis: the effect of varying basic wavelet parameters 总被引：4，自引：1，他引：3
The most commonly used methods to analyse (observed) quasi-periodic signals are standard techniques such as Fourier and wavelet analysis. Whereas a Fourier transform provides information on the dominant frequencies, wavelet analysis has the added advantage of providing the time localisation of the various frequency components. The usefulness and robustness of wavelet analysis is investigated by varying the different parameters which characterise the `mother' wavelet. We examine the effect of varying these parameters on the temporal and frequency resolution and the damping profile, which can be obtained from the wavelet transform. Additionally, the effect of a changing periodicity on the wavelet transform is investigated. Both simple harmonic functions and intensity oscillations observed by TRACE are used to demonstrate the various advantages and disadvantages of the different methods. In general, using the Paul wavelet or a smaller value of the wavelet parameter k provides a better time resolution, whereas the Morlet wavelet or a larger value of k improves the frequency resolution. Overall, our results indicate that great care is needed when using a wavelet analysis and that all the possible factors that could affect the transform should be taken into consideration. 相似文献
13.
In this work, we have simulated orbits of a particle moving in gravitational field of the Sun-Jupiter system. The effect of
solar radiation pressure, including Poynting Robertson drag, on the evolution of particle orbits in phase space have been
studied for different values of the parameter β
1 (the ratio of radiation to gravitational force) and initial conditions. Characteristics of various computed trajectories
have been studied using wavelet transform (WT), Fourier transform (FT) and Poincare surface of section method. We use wavelet
analysis to identify transitions of a trajectory in time-frequency plane and further apply it to classify it as regular or
chaotic in phase space. Unlike the Fourier transform method (FT), we observe that the wavelet transform (WT) also provides
a basis to identify ‘sticky’ trajectories in the present dynamical system. 相似文献
14.
We examine spectral time series of the transition region line Ov 629Å, observed with the Coronal Diagnostic Spectrometer (CDS) on the SOHO spacecraft in July 1997. Both Fourier and wavelet transforms have been applied independently to the analysis of plume oscillations in order to find the most reliable periods. The wavelet analysis allows us to derive the duration as well as the periods of the oscillations. Our observations indicate the presence of compressional waves with periods of 10–25 min. We have also detected a 11±1 min periodicity in the network regions of the north polar coronal hole. The waves are produced in short bursts with coherence times of about 30 min. We interpret these oscillations as outward propagating slow magneto-acoustic waves, which may contribute significantly to the heating of the lower corona by compressive dissipation and which may also provide enough energy flux for the acceleration of the fast solar wind. The data support the idea that the same driver is responsible for the network and plume oscillations with the network providing the magnetic channel through which the waves propagate upwards from the lower atmosphere to the plumes. 相似文献
15.
Hao-Jing Zhang Xiong Zhang Fu-Tong Dong Yong-Gang Zheng Ling Tang Li-Sheng Mao 《Chinese Astronomy and Astrophysics》2009
A kind of wavelet analysis method for identifying the light period of the BL Lac object S5 0716+714 is introduced. The rather complete observed data in the four optical wavebands B, V, R, I are collected, and the long-term light curves based on 10-day averaging are obtained. On these light curves, the periodicity analysis is performed by using a wavelet analysis method. The result demonstrates that the wavelet analysis method is preferable for searching and identifying the light periods of BL Lac objects. From the contour map of the real part of the wavelet transform coefficient, the periodical light variations of the BL Lac object S5 0716+714 can be precisely identified. By analyzing the wavelet variance curves at the 4 wavebands, it is found that the BL Lac Object S5 0716+174 has a stable light period of 1160 days. This result is consistent with the 3.3-year period given by Raiteri et al. It is predicted that the next outburst in this object will happen around the August of 2011. 相似文献
16.
Images and spectra contain a large amount of data. Therefore the question arises, how this data can be decreased or compressed without losing important detail. The discrete wavelet transform is a tool which can be used to compress data because of its good approximation properties. It is very easy to implement and requires approximately the same amount of calculation as the fast Fourier transform. It has the advantage of giving information both in time and frequency. Since most of the coefficients in the transformed data are very small compared to the maximum values, which means that they do not contribute much to the transform, a large number of them can be neglected. Although some data get lost, the physical results deduced from the data remain the same, as is demonstrated by various examples. By this method it is even possible to compress data containing much noise to high-compression ratios. 相似文献
17.
Ai-Ying Zhou 《Astrophysics and Space Science》2006,301(1-4):11-20
The variability of period and amplitude of the high-amplitude δ Scuti star YZ Boo was thoroughly investigated based on a comprehensive
analysis of new time-series photometry and other available data. Fourier analysis, O–Cdiagram, and wavelet analysis establish a clear picture for the star's time-dependent behavior in period and amplitude. We
detected no additional frequencies being intrinsic to the variable or caused by amplitude/frequency modulation confirming
its mono-periodicity. We reveal the pulsation of YZ Boo is quite stable in both period and amplitude over the past 50 years.
Short-term variations at cycle level including “anomalous cycles” are present clearly, while long-term variations in period
and amplitude at annual base are insignificant. However, we note an increment from 2000 to 2003 in both period and amplitude.
In 2000 the amplitude reached the lowest. This is indicated by the Fourier and wavelet results. In the long term, O–Cfits and wavelet analysis agree with the Fourier results that the period change of YZ Boo is still inconclusive. 相似文献
18.
时间尺度的分域递推模型 总被引：1，自引：0，他引：1
建立时间尺度是时间测量的目的之一．实时原子时则要求对时间尺度进行必要的预测．小波分析是近年来迅速发展起来的一门学科,它可以对信号在不同的分辨率下进行分析,凡是传统的Fourier分析可以应用的地方,小波分析都可以得到应用．基于小波分析建立了一种时间尺度分域递推模型,这种方法既不同于ARMA（p,q）模型,又有别于卡尔曼滤波方法．ARMA模型要求过程是平稳随机的,而卡尔曼滤波方法虽然不要求过程是平稳的,但它预测的精度有限．分城递推模型将信号在不同的频率尺度进行正交分解,在各个尺度上对小波变换系数进行建模．最后根据陕西天文台守时实验室的实测数据,验证了分域递推模型,ARMA模型一步预测误差10ns,而分域递推模型五步预测误差平均为4．5ns．结果表明这种方法简单而切实可行,分域递推模型的预测精度优于其它方法． 相似文献
19.
由单颗脉冲星定义的脉冲星时受多种噪声源的影响,其短期和长期稳定度都不够好.为了削弱这些噪声源对单脉冲星时的影响,可以采取合适的算法对多个单脉冲星时进行综合得到综合脉冲星时,从而提高综合脉冲星时的长期稳定度.文中介绍4种综合脉冲星时算法:经典加权算法、小波分析算法、维纳滤波算法和小波域中的维纳滤波算法,将这4种算法分别应用于Arecibo天文台对两颗毫秒脉冲星PSR B1855+09和PSRB1937+21观测得到的计时残差并作出比较. 相似文献
20.
Based on the DWT (discrete wavelet transform) method, we propose a new smoothing algorithm for computing surface densities from 3D numerical simulation samples. To check its effectiveness, we have applied this algorithm to two Monte-Carlo samples of gravitational lens simulation with different mass resolutions, generated from the isothermal ellipsoid model of dark matter halos. The calculated results indicate that this algorithm can reconstruct accurately the surface density distribution of the gravitational lens simulation sample, and that the lens caustics and critical curves derived from the surface densities agree well with the theoretical curves. We have compared the results calculated by using 3 different wavelet bases (Daub4, Daub6 and B-spline 3th), and identified the best one. Without sacrificing its smoothing capability, this algorithm has a very fast computing speed, suitable for later N-body numerical simulations, which require even higher resolutions. 相似文献