共查询到20条相似文献,搜索用时 108 毫秒
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时序资料的时间窗平滑法及应用 总被引:3,自引:0,他引:3
观测资料的平滑处理,是数据分析中一类重要的常用方法,平滑处理的目的,在于既保留资料中的主要有用信号,又消除或削弱随机误差,本文对密集采样时序资料,提出了时间窗平滑法,并以光谱和光电测量资料为例,通过分析PDM技术中拟合曲线的计算,说明了它的性质与应用,与高斯权函数平滑法相比,此方法计算简便,且有更明确的物理意义,与观测值多点合并法相比,有更好的采样一致性和避免损失实际的分辨率,当用于等间距时序资料 相似文献
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The X-ray nuclei of intermediate-redshift radio sources 总被引:2,自引:0,他引:2
M. J. Hardcastle D. A. Evans J. H. Croston 《Monthly notices of the Royal Astronomical Society》2006,370(4):1893-1904
We re-assess the question of a systematic time delay between the formation of the progenitor and its explosion in a Type Ia supernova (SN Ia) using the Hubble Higher- z Supernova Search sample. While a previous analysis indicated a significant time delay, with a most likely value of 3.4 Gyr, effectively ruling out all previously proposed progenitor models, our analysis shows that the time-delay estimate is dominated by systematic errors, in particular due to uncertainties in the star formation history (SFH). We find that none of the popular progenitor models under consideration can be ruled out with any significant degree of confidence. The inferred time delay is mainly determined by the peak in the assumed SFH. We show that, even with a much larger supernova sample, the time-delay distribution cannot be reliably reconstructed without better constraints on the SFH. 相似文献
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L.S. Slavcheva-Mihova V.L. Oknyanskij B.M. Mihov 《Astrophysics and Space Science》2001,275(4):385-389
We present the results of CCD photometry of the first gravitational lenssystem QSO 0957+561, obtained on the base of La Palma archive. Usingcross-correlation analysis we have found the time delay between A and Bquasar images to be 430 ± 15 days. Our photometry of QSO 0957+561 A & Bgives additional independent confirmation of the recent results on the time delay about 425 days. 相似文献
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Li-Feng Xing Xiao-Bin Zhang Jian-Yan Wei National Astronomical Observatories Chinese Academy of Sciences Beijing Department of Technology Physics Zhengzhou University of Light Industry Zhengzhou Graduate School of Chinese Academy of Sciences Beijing 《中国天文和天体物理学报》2006,6(6):716-722
We monitored the light curves of 22 weak-line T Tauri stars (WTTSs) discovered among the X-ray sources in the field of the Taurus-Auriga cloud. For 12 of the 22 WTTSs photometric periodic variability is confirmed and their rational periods are determined using Phase Dispersion Minimization (PDM) and Fourier analysis. Most of them are found to have periods shorter than one day. This gives further evidence for the spin up of solar-type stars predicted by the models of angular momentum evolution of pre-main sequence stars. 相似文献
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网络时延对网上高时间约束业务影响的讨论 总被引:1,自引:0,他引:1
给出了一系列的网络测量结果。通过对实测结果的分析,结合图表形象地揭示了网络时延的严重性、随机性和信息路径的不确定性,指出了这种网络现象对具有高时间约束的网络通信业务的严重影响,并阐述了测量和改正网络时延的重要意义。 相似文献
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K. E. McGowan P. A. Charles D. O'Donoghue A. P. Smale 《Monthly notices of the Royal Astronomical Society》2003,345(3):1039-1048
We have obtained high time resolution (seconds) photometry of LMC X-2 in 1997 December, simultaneously with the Rossi X-ray Timing Explorer ( RXTE ), in order to search for correlated X-ray and optical variability on time-scales from seconds to hours. We find that the optical and X-ray data are correlated only when the source is in a high, active X-ray state. Our analysis shows evidence for the X-ray emission leading the optical with a mean delay of <20 s. The time-scale for the lag can be reconciled with disc reprocessing, driven by the higher-energy X-rays, only by considering the lower limit for the delay. The results are compared with a similar analysis of archival data of Sco X-1. 相似文献
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Alice C. Quillen Joss Bland-Hawthorn 《Monthly notices of the Royal Astronomical Society》2008,386(4):2227-2234
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. 相似文献
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. 相似文献