钻孔施工对新丰江和平地电台深井地电阻率观测影响的数值模拟

1 观测背景 深井地电阻率观测在消除地表干扰、季节天气变化影响等方面效果良好(刘昌谋等, 1994),是当前地电阻率观测的发展趋势.广东新丰江和平地电台于1992年起开展深孔布极地电阻率观测,并在几次显著地震前观测到明显的异常变化.2015年3—5月,该台地电阻率测值出现显著异常变化,怀疑为测区钻孔施工对电阻率测值的变化起了决定性作用.为深入了解地电阻率变化的异常机理,在现场调查核实的基础上,收集数据资料建立测区电性结构有限元模型,采用数值模拟对异常进行定量分析,探讨钻孔施工对地电阻率观测的影响幅度与规律.     

摇摆-自复位桥墩的多弹簧模型建模方法研究

为探讨摇摆-自复位（Rocking Self-Centering,RSC）桥墩的滞回行为并为其数值建模提供依据,基于OpenSees地震分析平台发展此类结构的多弹簧模型并开展系统性讨论。结合RSC桥墩的构造特点发展多弹簧模型的整体建模思路,着重对比三种弹簧分布（基于Gauss积分和Lobatto积分的分布及均匀分布）模式下RSC桥墩的整体力-位移响应,对弹簧所需设置个数进行优化分析,并讨论了弹簧刚度的校准过程。最后,基于现有研究的5个RSC桥墩试件的试验结果,通过对比滞回曲线,发现所建议的模拟方法可较为准确地模拟RSC桥墩在拟静力荷载下的刚度、强度、滞回行为及残余位移。     

黄河中游砒砂岩地区长川流域土地利用变化分析

根据1976年的Landsat-MSS影像数据以及1987年和2000年的Landsat-TM影像数据,应用遥感和地理信息系统手段以及转移矩阵和景观空间格局指数分析方法,对地处黄河中游砒砂岩地区的内蒙古准格尔旗长川流域土地利用及其变化进行研究。结果表明：1)研究区内分布最多的土地利用类型是灌木林地、草地和难利用地,该三个土地利用类型的面积占研究区域总面积75％;2)从1976～2000年期间,虽然乔木和灌木林地的面积明显增加,但同时也存在林地和草地向难利用土地、沙地和农地的转变过程。与此同时水域亦明显减少;3)水土保持生物措施的实施、农田开垦和降雨量偏少可能是导致研究区土地利用变化的主要原因。     

基于解析梯度的近地小天体探测机会搜索问题研究木

研究近地小天体的探测机会搜索问题．针对交会型探测任务,通过结合变分理论和状态转移矩阵推导了性能指标关于可调参数的解析偏导数,然后在搜索空间中随机生成初始点,并从这些初始点出发利用解析偏导数寻优,从而得到搜索空间内对应潜在发射机会的全部局部极小值点．此方法既在一定程度上保持了传统搜索方法全局搜索的特点,又克服了传统搜索方法的盲目性,因此计算速度获得很大提高．此外该方法可以对探测机会的搜索精度进行有效地控制．     

基于解析梯度的近地小天体探测机会搜索问题研究

研究近地小天体的探测机会搜索问题.针对交会型探测任务,通过结合变分理论和状态转移矩阵推导了性能指标关于可调参数的解析偏导数,然后在搜索空间中随机生成初始点,并从这些初始点出发利用解析偏导数寻优,从而得到搜索空间内对应潜在发射机会的全部局部极小值点.此方法既在一定程度上保持了传统搜索方法全局搜索的特点,又克服了传统搜索方法的盲目性,因此计算速度获得很大提高.此外该方法可以对探测机会的搜索精度进行有效地控制.     

Observations of Giant Pulses of the Crab Pulsar

The Crab Pulsar was observed at 1540 MHz with the 25m radio telescope at Urumqi with a filterbank de-dispersion backend. A total of 2436 giant pulses with pulse energies larger than 4300 Jy μs were detected in two observing sets. All of these giant pulses are located in the main pulse (MP) and inter pulse (IP) windows of the average profile of the Crab Pulsar. The ratio of the numbers of giant pulses detected in the IP and MP windows is about 0.05. Our results show that, at 1540 MHz, the emission in the IP is contributed by giant and normal pulses, while that in the MP is almost dominated by giant pulses. The distribution of energy of the 2436 giant pulses at 1540 MHz can be described by a power-law with index α=3.13±0.09. The intrinsic threshold of giant pulse energy in the MP window is about 1400 Jy μs at 1540 MHz.     

The Effect of AGN and SNe Feedback on Star Formation, Reionization and the Near Infrared Background

Feedback from supernovae (SNe) and from active galactic nuclei (AGN) accom-panies the history of star formation and galaxy evolution. We present an analytic model to explain how and when the SNe and AGN exert their feedback effects on the star formation and galaxy evolution processes. By using SNe and AGN kinetic feedback mechanisms based on the Lambda Cold Dark Matter (LCDM) model, we explore how these feedback mecha-nisms affect the star formation history (SFH), the Near-Infrared Background (NIRB) flux and the cosmological reionization. We find the values of the feedback strengths, ∈AGN =1.0+0.50.3and ∈SN=0.04+0.02-0.02, can provide a reasonable explanation of most of the observational re-suits, and that the AGN feedback effect on star formation history is quite different from the SNe feedback at high redshifts. Our conclusions manifest quantitatively that these feedback effects decrease star formation rate density (SFRD) and the NIRB flux (in 1.4 - 4.0μm), and postpone the time of completion of the cosmological reionization.     

An X-Ray Study of Lobe-Dominated Radio-Loud Quasars with XMM-Newton

We report on our results of X-ray spectral analysis for a sample of radio-loud quasars covering a wide range of the radio core-dominance parameter, R, from core-dominated to lobe-dominated objects, using data obtained mostly with the XMM-Newton Observatory. We find that the spectral shape of the underlying power-law continuum is flat even for the lobe-dominated objects (average photon index ～ 1.5), indistinguishable from that of core-dominated quasars. For lobe-dominated objects, contribution of X-rays from the jets is expected to be very small based on previous unification schemes, more than one order of magnitude lower than the observed X-ray luminosities. Assuming that radio-loud quasars follow the same X-ray-UV/optical luminosity relation for the disk-corona emission as found for radio-quiet quasars, we estimate the X-ray flux contributed by the disk-corona component from the optical/UV continuum. We find that neither the luminosity, nor the spectral shape, of the disk-corona X-ray emission can account for the bulk of the observed X-ray properties. Thus in lobe-dominated quasars, either the disk-corona X-ray emission is much enhanced in strength and flatter in spectral shape (photon index～1.5) compared to normal radio-quiet quasars, or their jet X-ray emission is much enhanced compared to their weak radio core-jet emission. If the latter is the case, our result may imply that the jet emission in X-rays is less Doppler beamed than that in the radio. As a demonstrating example, we test this hypothesis by using a specific model in which the X-ray jet has a larger opening angle than the radio jet.     

太阳活动周期及其数学描述

概述和分析了太阳活动周期的研究进展,太阳活动呈现非常复杂的周期性,其周期性范围从几天至上百年,11年周期意义比较大,也比较明显;几天至几个月的周期性可能发生在太阳活动高峰期,155天或更短的周期存在,对中期预报有帮助;几年左右的周期对气象学的研究有作用;"蒙德极小期"是否存在至今还没有定论.对太阳活动11年周期的数学描述虽然很多,从效果上看,一般情况下,参数较多的函数计算量很大,误差相对较小;参数少的函数相比参数多的函数误差大,但计算量小;目前还没有一个非常理想的函数.能够对每个活动周都能很好的描述且误差很小.