中国大陆及邻区、川滇成组强震活动特征初步研究

将中国大陆及其邻区1902年以来MS≥7地震的成组活动划分出7组,其首发大震分别为1902年阿图什8.2级,1911年阿拉木图8.2级,1920年海原8.5级,1931年富蕴8.0级,1946年缅甸7.8级,1966年邢台7.2级,1988年缅甸7.2级。川滇MS≥6.7地震成组活动划分出5组,其首发强震为1913年峨山7.0级,1933年茂县7.5级,1948年理塘7.3级,1966年东川6.5级、6.2级,1988年澜沧7.4级。其中,川滇MS≥7的首发大震滞后中国大陆首发大震几个月至4年不等。按成组大震的界定,目前中国大陆处于1998~2007年(估计)的大震少发时段。川滇未来1~2年的大震形势为川滇西部存在发生大震的可能性。中国大陆新一轮强震成组活动中的大地震将可能在2007~2009年前后发生,主体危险区可能为天山地震带中段及川滇东部。2007~2008年可能出现5~6级地震的增强过程。巧家—东川一带可能最先发生6级地震。     

Statistical features of aftershock distribution size for moderate and large earthquakes in Chinese mainland

Based on data of earthquake sequences with MS≥5.0 in Chinese mainland from 1970 to 2004,for different se-quence types and different rupture modes of the main shock,the relationship between aftershock distribution size Rand the magnitude of the main shock M0 has been studied statistically.Considering the rupture mode of the mainshock,we give the quantitative statistical relationships between R and M0 under 95%confidence level for differentsequence types.Qualitatively,lgR,the logarithm of the aftershock distribution size,is positively correlative to theM0,but the data distribution is dispersed.Viewing from different sequence types,the correlation between R and M0is very weak for isolated earthquake type(IET)sequence,R distributes in the range from 5 to 60 km;For main-shock-aftershock type(MAT),lgR is positively correlative to M0;For multiple main shock type(MMT),the core-lation between lgR and M0 is not very obvious when M0≤6.2 and R distributes in the range from 5 to 70 km,whileit shows a linear correlation when M0≥6.3.The statistical results also show that the occupational ratios of differentsequence types for strike-slip and oblique slip are almost the same.But for dip-slip(mostly are thrust mechanisms),the ratio of MAT is higher than that of IET and MMT.Comparing with previous results,it indicates that,when M0is large enough,R is mainly determined by M0 and there is almost no relationship with the rupture mode of themain shock.     

中国大陆中强以上地震余震分布尺度的统计特征

依据1970年以来记录相对完备的MSge;5.0地震序列资料，统计研究了中国大陆余震分布尺度与序列最大地震震级M0及最大地震破裂形式之间的关系. 在95%置信概率下，考虑主震破裂形式， 分序列类型给出了余震分布尺度与M0之间的统计关系. 定性而言，余震分布尺度的对数lgR与M0正相关， 但数据分布较为离散. 分类型来看， 孤立型序列余震分布尺度与M0之间统计相关程度低， 余震分布尺度介于5~60 km之间； 主余型序列lgR与M0正相关； 多震型序列当M0le;6.2时lgR与M0之间相关性不显著，余震分布尺度介于5~70 km之间， 当M0ge;6.3时lgR与M0线性相关. 统计结果还表明， 走滑近走滑及斜滑型主震所导致序列类型比例之间没有显著差异，而倾滑近倾滑型主震（主要为逆断型破裂）所导致的主余型序列所占比例较高， 孤立型及多震型序列所占比例则相对较低. 对比研究显示， 当M0较高时，余震分布尺度主要取决于主震大小而与主震破裂形式关系不明显.      

斜拉桥索塔三维相对基准定位方法研究

结合斜拉桥索塔基准放样及斜拉索预埋钢管的精密定位的需要，提出了一种新的基于测量机器人的三维相对基准放样方法，并成功用于灌河特大桥斜拉桥主桥的施工放样。实践证明，与传统的方法相比，该方法具有方便、高效、精度高等特点。     

简单剪切——中国活动构造变形主要机制

采用简单剪切对中国活动的构造组合进行解译,提出简单剪切是主要变形机制,着重对简单剪切依据进行了论述,对简单剪切与老构造的关系作了初步讨论,提出需要继续探讨的主要问题。     

找出最主要的控矿因素,建立三因控矿分析思路

通过几个已知金矿区的研究,认为到不同矿区有不同的控矿因素,首先找出最主要的控矿因素,再配合两个深层相关因素,进行矿体定位。     

基于主成分分析的库存管理神经网络模型研究

从影响合理库存的诸多因素中,利用数理统计的思想,找出若干主要指标,通过建立神经网络模型,进行模拟仿真,寻求一种解决问题的有效方法,把库存调整到理想的状态。     

Chemical spots on the surface of the strongly magnetic Herbig Ae star HD 101412

Due to the knowledge of the rotation period and the presence of a rather strong surface magnetic field, the sharp‐lined young Herbig Ae star HD 101412 with a rotation period of 42 d has become one of the most well‐studied targets among the Herbig Ae stars. High‐resolution HARPS polarimetric spectra of HD 101412 were recently obtained on seven different epochs. Our study of the spectral variability over the part of the rotation cycle covered by HARPS observations reveals that the line profiles of the elements Mg, Si, Ca, Ti, Cr, Mn, Fe, and Sr are clearly variable while He exhibits variability that is opposite to the behaviour of the other elements studied. Since classical Ap stars usually show a relationship between the magnetic field geometry and the distribution of element spots, we used in our magnetic field measurements different line samples belonging to the three elements with the most numerous spectral lines, Ti, Cr, and Fe. Over the time interval covered by the available spectra, the longitudinal magnetic field changes sign from negative to positive polarity. The distribution of field values obtained using Ti, Cr, and Fe lines is, however, completely different compared to the magnetic field values determined in previous low‐resolution FORS 2 measurements, where hydrogen Balmer lines are the main contributors to the magnetic field measurements, indicating the presence of concentration of the studied iron‐peak elements in the region of the magnetic equator. Further, we discuss the potential role of contamination by the surrounding warm circumstellar matter in the appearance of Zeeman features obtained using Ti lines. (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

遥感干旱应用技术进展及面临的技术问题与发展机遇

干旱是全球各地区普遍存在的一种气候现象,也是对人类社会影响最为严重的一种自然灾害。全球气候变化和社会发展加剧了干旱的影响程度,增强了干旱灾害的风险,给全球农业、水资源、生态环境安全以及社会可持续发展造成巨大威胁,提高干旱监测和早期预警技术水平是应对、管理干旱和减轻干旱脆弱性的基础。近30 a来随着全球对地观测技术的迅速发展,卫星遥感监测干旱技术取得很大进步,在全球干旱监测和早期预警中发挥着不可替代的作用。但是,干旱是多学科交叉的复杂问题,其发展过程缓慢、时间和空间表现特征差异很大,遥感监测干旱技术在应用中还存在许多技术问题,对抗旱防灾提供支撑的力度仍不够。本文在简要总结卫星遥感监测干旱应用技术的基础上,对各种指数(模型)应用中存在的问题进行评述,指出卫星遥感干旱监测面临的主要技术问题和未来发展机遇;针对我国卫星遥感干旱应用现状,提出了亟待解决的主要问题和应该努力的方向。     

Finding the most variable stars in the Orion Belt with the All Sky Automated Survey

We look for high‐amplitude variable young stars in the open clusters and associations of the Orion Belt. We use public data from the ASAS‐3 Photometric V ‐band Catalogue of the All Sky Automated Survey, infrared photometry from the 2MASS and IRAS catalogues, proper motions, and the Aladin sky atlas to obtain a list of the most variable stars in a survey area of side 5° centred on the bright star Alnilam (ε Ori) in the centre of the Orion Belt. We identify 32 highly variable stars, of which 16 had not been reported to vary before. They are mostly variable young stars and candidates (16) and background giants (8), but there are also field cataclysmic variables, contact binaries, and eclipsing binary candidates. Of the young stars, which typically are active Herbig Ae/Be and T Tauri stars with Hα emission and infrared flux excess, we discover four new variables and confirm the variability status of another two. Some of them belong to the well known σ Orionis cluster. Besides, six of the eight giants are new variables, and three are new periodic variables (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)