中国东北完达山地区早白垩世同构造岩浆侵位——对晚中生代左行走滑作用的响应

分布于中国东北完达山地区的饶河花岗岩岩体中暗色矿物和斑晶钾长石定向排列,呈北北东走向,其中透镜状闪长质捕掳体近水平排列,局部具有左行剪切的特点。岩体中发育石香肠状石英脉,表明岩体在侵位过程中受到左行剪切作用的影响或制约。对出露的花岗岩进行LA-ICP-MS锆石U-Pb定年,获得年龄121±1Ma和119±1Ma,表明该岩浆流动形成于早白垩世。同时对围岩辉长岩、侵入岩体中的正长岩脉和辉绿岩脉进行锆石U-Pb年龄分析,分别获得160±1Ma、109±2Ma、124±1Ma的年龄结果。根据各样品中继承锆石的特征,围岩辉长岩的年龄数据很集中,不存在古老锆石的年龄信息。岩浆流动岩体及岩脉中都有太古宙、元古宙等各时代的锆石年龄数据,可能表明完达山地区在约120Ma之前已完成古太平洋板块的俯冲拼贴,饶河岩体形成于走滑环境下的陆内变形,为同构造侵入岩。     

全国天文大地网各类方向观测值之权的检定

为了检验和评定我国天文大地网各类方向观测值之权的合理性和正确性,本文给出了两种方法:1、由赫尔默特的简化计算公式,以估算各类方向观测值的方差和它们的权的最佳估值;2、在一定精度要求下求定各类方向观测值的权的选取范围。通过计算和分析,我们认为:我国天文大地网平差时给出的各类方向观测值的权P_i是较为合理的。     

Terrestrial surface-area increment: the effects of topography,DEM resolution,and algorithm

The area increment of land surface compared with its projected area is an effect of topographic relief and is also a source of environmental variations. To examine the effects of topography and data resolution on surface area calculation, we calculated incremental area coefficients (IACs), based on two different algorithms, for a DEM of China at a series of spatial resolutions. Sampling the DEM with a regional network of 50?km?×?50?km cell size, we explored the relationships among the two IACs and topographic features. Both IACs studied were exponential functions of resolution. At 30-m resolution, the IACs were 4.31 and 4.89% over China, respectively. The largest increment for a 50?km?×?50?km cell was >45%. Between the IACs there was a linear relationship that varied with DEM resolution. Hierarchical variation partitioning revealed that the factors included contributed in a very similar percentage composition to the two IACs, mean slope (37.5 or 38.7%) and standard deviation of slope (22.3 or 19.6%) at local scale dominated the area increment, followed by regional elevation range. Data resolution contributed about 10%, while the deviation of slope exposure only had minimal (1.4 or 1.7%) impact on surface-area increment. For a specific type of geomorphology, a threshold resolution of DEM can be determined, below which the surface-area increment (i.e., IAC) is negligible. Our results provided the first comprehensive estimate of the contributions of the topographic features, DEM resolution, and algorithms for the surface-area increment, and indicated the scale-related properties and potential environmental consequences of topographic heterogeneity in various estimates of natural resources and ecosystem functions when area needs to be taken into account.     

Long-term seismic noise investigations on Shikotan Island: First results

In 2003–2004, long-term seismic noise observations were launched on Shikotan Island (Lesser Kuril Range) based on the “Shikotan” dormant regional seismic station. The geological and geophysical data on the registration area are reported. Information about the equipment and its technical specifications is given. The precursors to the strongest local earthquakesthat occurred in the Shikotan Island region in January 2005–March 2007 are identified.     

土地利用对溶丘洼地土壤容重、水分和有机质空间异质性的影响——以南洞流域驻马哨洼地为例

为了探究溶丘洼地土壤空间异质性及其影响因素,本文以驻马哨溶丘洼地为研究对象,利用经典统计学和地统计学的方法,从不同土地利用、坡度、坡向、土壤深度分析土壤容重、水分及有机质的空间异质性。结果表明:（1）土壤有机质为强变异,变异系数为0.71,容重和水分变异系数分别为0.15、0.11,属中等变异,土壤容重和水分呈极显著负相关,和有机质呈显著负相关,相关系数分别为-0.609、-0.581;（2）块基比介于0.78~0.97,随机部分引起的空间变异程度较大,空间自相关较小,且模型拟合较好。（3）耕地土壤有机质、水分含量最低,容重最大,而灌木土壤反之;（4）北坡土壤容重高于南坡,变异系数小于南坡;而土壤水分、有机质低于南坡,变异系数高于南坡。从不同坡位、坡向的比较中,皆体现了土地利用对土壤空间异质性的影响。在土地利用作为主要因素的影响下,驻马哨洼地土壤水分、容重、有机质由随机部分引起的空间变异增加,空间自相关减小。      

湖北省山区与平原雷电分布及其参数特征

为进一步了解山区与平原雷电参数分布特征及其差异,为山区和平原地区雷电防护工程设计和雷击风险评估提供参考,根据湖北省ADTD地闪定位系统2006年12月至2016年12月监测的资料,采用数理统计方法,对山区和平原地区的地闪频次、极性、雷电流幅值和波头陡度等参数分布特征进行了对比研究。结果表明:①山区地闪密度略高于平原地区,平原正地闪百分比稍高于山区,近10年的正地闪百分比呈上升趋势。②正地闪平均强度山区比平原大1.16kA,负地闪平均强度山区比平原小3.67kA,平原总地闪平均强度比山区大3.46kA。③总地闪小雷电流幅值(I≤30kA)概率山区比平原大8.9%,大雷电流幅值(I100kA)概率平原比山区大0.6%。④山区正地闪平均陡度分别比负、总地闪平均陡度大2.44kA/μs和2.31kA/μs,平原正、负、总地闪平均陡度分别比山区大3.41kA/μs、5.77kA/μs和5.64kA/μs。可以得出,山区小雷电流绕击率大于平原,正地闪雷电感应的危害大于负地闪和总地闪;平原地区大雷电流反击率比山区大,雷电感应的危害大于山区。     

THE INFLUENCE OF HORIZONTALLY NON-UNIFORM HEATING UPON THE DEVELOPMENT OF STRONG CONVECTIVE MESOSCALE DISTURBANCES

It is shown by observational data and synoptic analysis that the development of strong convective echo is influenced by the horizontally non-uniform heating, such as the one caused by lake-land distribution. In this paper, a simple linear cell-convection model is established using an appropriate heating field, and the instability of heating convection is theoretically studied. It is found that the heating convection development will be unstable if the heating-caused temperature gradient dT0/dy is greater than the critical value (dT0/dy)c which is approximately 0.64℃/10 km, and that the development of convective band has a preferred width of 12.5 km. It will take 25 min for the initial disturbance to increase intensity by 10 times. All these results are in rather good agreement with the squall line process in the lake-land region of Jiangsu Province on June 8, 1979.     

Incoherent radiation from relativistic electrons with power energetic spectrum

It is shown that an incoherent high-frequency radiation from an ensemble of relativistic particles with the power energy distribution is described by a certain general expression which covers practically all the cases of particle radiation in random electromagnetic fields of cosmic radiation sources.     

黄河下游及河口区超铀元素Pu的浓度测定

本文测定研究了黄河口及下游区表层沉积物中的Pu浓度。结果表明,该区表层沉积物中存在微量的Pu污染;黄河口的Pu浓度高于下游区;该区的Pu,~(137)Cs两个同位素有相似的变化规律。     

X-ray activity from different types of stars

X-ray emission is an important indicator of stellar activity. In this paper, we study stellar Xray activity using the XMM-Newton and LAMOST data for different types of stars. We provide a sample including 1259 X-ray-emitting stars, of which 1090 have accurate stellar parameter estimations. Our sample size is much larger than those used in previous works. We find a bimodal distribution of the X-ray to optical flux ratio(log(fX/fV)) for G and K stars. We interpret that this bimodality is due to two subpopulations with different coronal heating rates. Furthermore, using the full widths at half maxima calculated from Hα and Hβ lines, we show that these stars in the inactive peaks have smaller rotational velocities. This is consistent with the magnetic dynamo theory that presumes stars with low rotational velocities have low levels of stellar activity. We also examine the correlation between log(fX/fV) and luminosity of the excess emission in the Hα line, and find a tight relation between the coronal and chromospheric activity indicators.