地震活动热红外异常的影响因素分析

对地表热红外辐射的基础理论和各类地物的热红外辐射特性进行了简略介绍;对地形地貌、地物类型和气象等非震因素对地表热红外辐射的影响及地表热红外亮温的时空变化特征进行了详细的分析;对各类非震因素的去除方法进行了探讨。初步认为,充分研究活动构造区带在各类非震因素影响下的热红外影像特征,掌握无震条件下的红外亮温时空演化过程,建立红外亮温变化的基准模型及各类非震因素的扣除模型,将有可能较好地排除非震因素的影响,检测出与地震活动有关的热异常。     

红河断裂带两侧地块地震震源参数研究

利用云南区域数字地震遥测台网资料,采用Brune圆位错模型对1998年12月至2006年8月云南境内M≥3地震和越南北部M>2地震测算震源参数。结果表明,红河断裂两侧活动块体的地震活动和震源参数存在较为明显的差异。就地震矩与震级的标度关系而言,滇西南块体与美国加州圣安德列斯断层和滇西实验场及其周边地区的结果一致,但与华南块体和越南北部地区有差异;从应力降的测算结果看,华南块体西缘的云南及越南北部地区的年均值为7.29MPa,滇西南块体为4.48MPa,两块体北部地震的应力降大于南部地区,应力降由北向南逐渐减小;就地震位错年均值而言,华南块体为12.3mm/a,滇西南块体为6.6mm/a。     

地质动力区划中断裂活动性的模糊综合评判

地质构造尤其是活动断裂控制着动力现象的区域性分布,然而活动断裂与矿井动力现象的关系并不是绝对和完全的。对断裂活动性进行评价,确定断裂的动力活动强度,是进行动力现象的预测与预防的重要内容之一。文章通过分析活动断裂的特征及其对矿区原地应力场的影响,提出了既具有代表性又容易获取的适合多尺度断裂活动性评价的5个主要指标,即活动断裂两侧断块的高程差、活动断裂长度、活动断裂走向与最大主应力的夹角、活动断裂走向与最大剪应力的夹角及断裂地震综合指标。利用模糊数学方法,建立了断裂活动性评价的模糊综合评判模型,确定了隶属函数,并通过层次分析法确定了各个指标的权重,最终获得了断裂活动性的模糊综合评判结果。将该方法应用于新汶矿区协庄矿,结果显示冲击地压多发生于具有强活动性的断裂附近。表明文章建立的评判模型能够较好地对断裂活动性进行分级。文章提出的模糊综合评判方法,改进了地质动力区划中断裂活动性评价方法,提高了评价结果的准确性及合理性。     

磁法在煤火探测中的应用

对采自宁夏汝箕沟煤田上覆盖层的原岩样品在温度作用下的磁性变化进行了系统研究.通过分析煤火区不同燃烧阶段围岩的温度变化情况,对原岩样品进行了模拟“燃烧”试验,试验结果表明,岩石磁性在不同温度作用条件下存在明显差异,从而从岩石磁性的角度讨论了磁法勘探圈定煤田火烧区的可行性.最后,采用人机交互法对地面实测磁异常剖面进行反演,有效地圈定了煤火区着火点的位置及范围.     

采用锚固和支撑与新型防护网SNS联合治理黄山风景区云汤线危岩崩塌

将传统的支撑锚固与新型SNS边坡防护技术应用于危岩的治理工程,不但解决了大块危岩治理问题,还解决了松动而无法清除危岩的崩落、掉块问题,且对自然景观破坏小,对旅游公路运营影响小,解决了场地狭窄与工程安全的矛盾,施工方便迅速,工程安全可靠。     

地震次生火灾研究进展

由于双重灾种叠加，地震次生火灾曾经带来过巨大生命财产损失，并始终严重威胁人类社会。梳理历史上几次重大地震次生火灾情况，归纳地震次生火灾的成灾与蔓延研究成果，讨论现有研究成果中常用的分析手段和研究方法；从工程结构和装备设施，以及灾害区划单元两个层面总结分析了地震次生火灾的风险与损失评估研究成果；从民用建筑、油气化工设施、核电站、灾后安置点与林业等多个方面探讨地震次生火灾的预防和控制研究进展。采用文献计量学方法对近二十年以"地震次生火灾"为主题的中文文献进行统计，并分析研究热度与地震事件的联系。     

The complex gravitational lens system B1933+503

We report the discovery of the most complex arcsec-scale radio gravitational lens system yet known. B1933+503 was found during the course of the CLASS survey and MERLIN and VLA radio maps reveal up to 10 components. Four of these are compact and have flat spectra; the rest are more extended and have steep spectra. The background lensed object appears to consist of a flat-spectrum core (quadruply imaged) and two compact 'lobes' symmetrically disposed relative to the core. One of the lobes is quadruply imaged while the other is doubly imaged. An HST observation of the system with the WFPC2 shows a galaxy with an axial ratio of 0.5, but none of the images of the background object is detected. A redshift of 0.755 has been measured for the lens galaxy.     

Cluster–subcluster mergers and the formation of narrow-angle tailed radio sources

We examine the ROSAT PSPC X-ray properties of a sample of 15 Abell clusters containing 23 narrow-angle tailed (NAT) radio galaxies. We find that clusters with NATs show a significantly higher level of substructure than a similar sample of radio-quiet clusters, indicating that NAT radio sources are preferentially located in dynamically complex systems. Also, the velocity distribution of the NAT galaxies is similar to that of other cluster members; these velocities are inadequate for producing the ram pressure necessary to bend the radio jets. We therefore propose a new model for NAT formation, in which NATs are associated with dynamically complex clusters undergoing merger events. The U -shaped NAT morphology is produced in part by the merger-induced bulk motion of the ICM bending the jets.     

Optical and near-infrared imaging of faint Gigahertz Peaked Spectrum sources

A sample of 47 faint Gigahertz Peaked Spectrum (GPS) radio sources selected from the Westerbork Northern Sky Survey (WENSS) has been imaged in the optical and near-infrared, resulting in an identification fraction of 87 per cent. The R  −  I R  −  K colours of the faint optical counterparts are as expected for passively evolving elliptical galaxies, assuming that they follow the R -band Hubble diagram as determined for radio-bright GPS galaxies. We find evidence that the radio spectral properties of the GPS quasars are different from those of GPS galaxies. The observed distribution of radio spectral peak frequencies for GPS sources optically identified with bright stellar objects (presumably quasars) is shifted compared with GPS sources identified with faint or extended optical objects (presumably galaxies), in the sense that a GPS quasar is likely to have a higher peak frequency than a GPS galaxy. This means that the true peak frequency distribution is different for the GPS galaxies and quasars, because the sample selection effects are independent of optical identification. The correlation between peak frequency and redshift that has been suggested for bright sources has not been found in this sample; no correlation exists between R magnitude (and therefore redshift) and peak frequency for the GPS galaxies. We therefore believe that the claimed correlation is actually caused by the dependence of the peak frequency on optical host, because the GPS galaxies are generally at lower redshifts than the quasars. The difference in the peak frequency distributions of the GPS galaxies and quasars is further evidence against the hypothesis that they form a single class of object.     

A search for optical polarization from the narrow-line Seyfert 1 galaxy RE J1034+396

We present spectropolarimetry data on RE J1034+396, an ultra-soft X-ray narrow-line Seyfert 1 galaxy, and find an upper limit of ∼ 0.4 to the linear polarization in the optical band. This suggests that there is no synchrotron emission in this AGN, and thus it is unlikely that RE J1034+396 is related to BL Lac objects. Furthermore, any other polarization arising from transmission through dust, or reflection from dust and electrons, must be cancelled out by geometrical effects or diluted to a high degree by unpolarized radiation.