基于时间序列分析和灰色理论的建筑物沉降预测模型研究

基于时间序列分析方法建立建筑物沉降预测模型,其中通过二次移动平均法提取出沉降监测序列中的趋势项,并在此基础上采用灰色系统理论动态GM（1,1）模型进行趋势项预测。实际算例结果表明,该模型能够较好地预测沉降变化的发展趋势,并具有较高的预测精度,证明了该预测模型具有一定的可行性和有效性。     

“天绘一号”卫星测绘相机在轨几何定标

卫星在空间环境运转过程中, 测绘相机的几何参数会发生不可预估的变化, 从而对摄影测量定位精度和数据处理精度产生影响。因此, 所有测绘卫星都对星载相机的几何参数进行在轨定标, 监测相机几何参数在轨运行状态下的变化情况。本文着重介绍了“天绘一号”卫星在轨几何定标的内容和采用的方法。     

“天绘一号”卫星在轨性能评估

“天绘一号”卫星是中国新一代传输型摄影测量卫星, 由航天东方红卫星有限公司基于CAST2000小卫星平台研制。01星于2010年8月发射成功, 02星于2012年5月发射成功。经过在轨测试, 两颗卫星性能指标均达到设计要求。本文介绍了“天绘一号”卫星在轨性能测试的结果, 为该卫星后续业务化应用提供宝贵数据。     

The Antarctic oscillation-East Asian summer monsoon connections in NCEP-1 and ERA-40

Connections between the spring Antarctic Oscillation(AAO)and the East Asian summer monsoon (EASM)in two reanalysis datasets—NCEP-1(NCEP/NCAR Reanalysis 1)and ERA-40(ECMWF 40- year Reanalysis)—are investigated in this study.Both show significant correlation between AAO and EASM rainfall over the Yangtze River valley,especially after about 1985.Though ERA-40 shows weaker anomalous signals connecting AAO and EASM over southern high latitudes than NCEP-1,both datasets reveal similar connecting patterns between ...     

地球系统10~(-1)年变化原因概述

我们曾论述了地球系统100～108年变化的原因[1], 唯对10-1年（月一年）的地球系统变化未指出其变化原因。经过近年的研究, 现在可以明确地指出, 地球内部有两类流体： 地外核和岩石圈裂隙中地下流体（地气）的活动是引发10-1年地球系统变化的原因。外核的上升运动会使其上部岩石圈产生上抬和压缩, 在地表层就出现3.2 m地温升高和降水减少的“干热异常”, 经过“孕震三步曲”最终引发构造地震。外核的下降运动会使其上部岩石圈产生下沉和拉张作用, 地表层表现为3.2 m地温降低, 同时降水增多的“湿冷异常”, 最终可导致发生陷落地震。外核的脉冲运动是引发岩石圈中形成地热（冷）涡的“源”。地气环流也是旋转地球上的一种流体运动, 其特征速度（地下风速）约为0.2 m/s, 据此可推得“自然气候周期”约为8个月。地气环流是使地气系统得以“流”的动力源。地热（冷）涡的“源”、 “流”相结合是使短期气候呈现纷繁复杂变化的原因。     

New magnetic field measurements of β Cephei stars and slowly pulsating B stars

We present the results of the continuation of our magnetic survey with FORS 1 at the VLT of a sample of B‐type stars consisting of confirmed or candidate β Cephei stars and Slowly Pulsating B (hereafter SPB) stars, along with a small number of normal B‐type stars. A weak mean longitudinal magnetic field of the order of a few hundred Gauss was detected in three β Cephei stars and two stars suspected to be β Cephei stars, in five SPB stars and eight stars suspected to be SPB stars. Additionally, a longitudinal magnetic field at a level larger than 3σ has been diagnosed in two normal B‐type stars, the nitrogen‐rich early B‐type star HD 52089 and in the B5 IV star HD 153716. Roughly one third of β Cephei stars have detected magnetic fields: Out of 13 β Cephei stars studied to date with FORS 1, four stars possess weak magnetic fields, and out of the sample of six suspected β Cephei stars two show a weak magnetic field. The fraction of magnetic SPBs and candidate SPBs is found to be higher: Roughly half of the 34 SPB stars have been found to be magnetic and among the 16 candidate SPBs eight stars possess magnetic fields. In an attempt to understand why only a fraction of pulsating stars exhibit magnetic fields, we studied the position of magnetic and non‐magnetic pulsating stars in the H‐R diagram. We find that their domains in the H‐R diagram largely overlap, and no clear picture emerges as to the possible evolution of the magnetic field across the main sequence. It is possible that stronger fields tend to be found in stars with lower pulsating frequencies and smaller pulsating amplitudes. A somewhat similar trend is found if we consider a correlation between the field strength and the v sin i ‐values, i.e. stronger magnetic fields tend to be found in more slowly rotating stars (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

The C1XS X-ray Spectrometer on Chandrayaan-1

The Chandrayaan-1 X-ray Spectrometer (C1XS) is a compact X-ray spectrometer for the Indian Space Research Organisation (ISRO) Chandrayaan-1 lunar mission. It exploits heritage from the D-CIXS instrument on ESA's SMART-1 mission. As a result of detailed developments to all aspects of the design, its performance as measured in the laboratory greatly surpasses that of D-CIXS. In comparison with SMART-1, Chandrayaan-1 is a science-oriented rather than a technology mission, leading to far more favourable conditions for science measurements. C1XS is designed to measure absolute and relative abundances of major rock-forming elements (principally Mg, Al, Si, Ca and Fe) in the lunar crust with spatial resolution ?25 FWHM km, and to achieve relative elemental abundances of better than 10%.     

A Study on the Long-term Spectral Variability of the Black-hole Candidate X-ray Binary Cyg X-1

Using the All-Sky Monitor (ASM, 1.5–12–kev) data of Rossi X-ray Timing Explorer (RXTE) from January 1996 to May 2005, we have made a detailed analysis of the correlation between photon-count rate and spectral hardness ratio HR2 (5–12 keV/3–5 keV) of the black-hole candidate X-ray binary Cyg X-1 in 3 energy bands, namely the A-band (1.5–3 keV), B-band (3–5 keV) and Cband (5–12 keV). By the study on the ASM data of 1-day time scale, we find: (1) When Cyg X-1 is in the soft state, the A-band photon-count rate and hardness ratio HR2 exhibit an anticorrelation, but in B-band and C-band there appears the positive correlation. When Cyg X-1 is in hard state, the photon-count rates in the A,B,C bands are all inversely correlated with the hardness ratio HR2; (2) No matter whether Cyg X-1 is in the soft state or the hard state, the hardness ratios HR2 and HR1 are always positively correlated. In addition, we have analyzed the “dwell by dwell” data of the ASM, and obtained the following interesting results: (1) In the period of MJD = 52600–52760 (while Cyg X-1 is in the hard state), the photon-count rates in the A-band and B-band are inversely correlated with HR2, but in the C-band there appears a relatively strong positive correlation; (2) During the hard state, a clear anticorrelation exists between the hardness ratios HR2 and HR1.     

New doubly-symmetric families of comet-like periodic orbits in the spatial restricted (N + 1)-body problem

For any positive integer N ≥ 2 we prove the existence of a new family of periodic solutions for the spatial restricted (N +1)-body problem. In these solutions the infinitesimal particle is very far from the primaries. They have large inclinations and some symmetries. In fact we extend results of Howison and Meyer (J. Diff. Equ. 163:174–197, 2000) from N = 2 to any positive integer N ≥ 2.