深井硬岩矿山岩爆灾害防治研究

采用室内试验、数值计算和现场岩爆研究相结合的综合研究方法,以冬瓜山矿床开采为对象,对深井矿床开采岩爆防治进行了系统的研究.由矿岩力学试验,采用岩爆综合评判指标确定了矿岩的岩爆倾向性,指出岩爆倾向性具有本源性和诱导性两种属性;电镜试验、物理模型试验和现场岩爆研究发现岩爆主要由张拉断裂引起,具有明显的岩石破坏和工程施工异常性前兆;现场岩爆研究和数值计算表明岩爆危险区位于应力集中、能量贮存大及具有快速释放能力和条件的区域;从岩爆预防角度,采用数值分析方法以能量释放率为衡量指标,对采场结构参数、开采步骤等进行了优化;从减少能量贮存、控制能量释放、采用柔性支护和建立岩爆监测系统4个方面,得出了具体的岩爆防治措施.图3,表2,参11.     

The afterglow and elliptical host galaxy of the short gamma-ray burst GRB 050724

Despite a rich phenomenology, gamma-ray bursts (GRBs) are divided into two classes based on their duration and spectral hardness--the long-soft and the short-hard bursts. The discovery of afterglow emission from long GRBs was a watershed event, pinpointing their origin to star-forming galaxies, and hence the death of massive stars, and indicating an energy release of about 10(51) erg. While theoretical arguments suggest that short GRBs are produced in the coalescence of binary compact objects (neutron stars or black holes), the progenitors, energetics and environments of these events remain elusive despite recent localizations. Here we report the discovery of the first radio afterglow from the short burst GRB 050724, which unambiguously associates it with an elliptical galaxy at a redshift z = 0.257. We show that the burst is powered by the same relativistic fireball mechanism as long GRBs, with the ejecta possibly collimated in jets, but that the total energy release is 10-1,000 times smaller. More importantly, the nature of the host galaxy demonstrates that short GRBs arise from an old (> 1 Gyr) stellar population, strengthening earlier suggestions and providing support for coalescing compact object binaries as the progenitors.     

A giant gamma-ray flare from the magnetar SGR 1806-20

Two classes of rotating neutron stars-soft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars-are magnetars, whose X-ray emission is powered by a very strong magnetic field (B approximately 10(15) G). SGRs occasionally become 'active', producing many short X-ray bursts. Extremely rarely, an SGR emits a giant flare with a total energy about a thousand times higher than in a typical burst. Here we report that SGR 1806-20 emitted a giant flare on 27 December 2004. The total (isotropic) flare energy is 2 x 10(46) erg, which is about a hundred times higher than the other two previously observed giant flares. The energy release probably occurred during a catastrophic reconfiguration of the neutron star's magnetic field. If the event had occurred at a larger distance, but within 40 megaparsecs, it would have resembled a short, hard gamma-ray burst, suggesting that flares from extragalactic SGRs may form a subclass of such bursts.     

Detection of bursts in neuronal spike trains by the mean inter-spike interval method

Bursts are electrical spikes firing with a high frequency, which are the most important property in synaptic plasticity and information processing in the central nervous system. However, bursts are difficult to identify because bursting activities or patterns vary with physiological conditions or external stimuli. In this paper, a simple method automatically to detect bursts in spike trains is described. This method auto-adaptively sets a parameter (mean inter-spike interval) according to intrinsic properties of the detected burst spike trains, without any arbitrary choices or any operator judgment. When the mean value of several successive inter-spike intervals is not larger than the parameter, a burst is identified. By this method, bursts can be automatically extracted from different bursting patterns of cultured neurons on multi-electrode arrays, as accurately as by visual inspection. Furthermore, significant changes of burst variables caused by electrical stimulus have been found in spontaneous activity of neuronal network. These suggest that the mean inter-spike interval method is robust for detecting changes in burst patterns and characteristics induced by environmental alterations.     

金纹细蛾的生物学特性及防治研究

金纹细蛾在河北冀东地区一年发生 5代 ,以蛹越冬 ,主要以幼虫潜食植物叶肉为害。各代成虫发生盛期分别为 :越冬代 4月 15～ 18日 ;第一代 5月 2 3～ 2 8日 ;第二代 6月 2 2～ 7月 2日 ;第三代 7月 2 0日～ 8月5日 ;第四代 8月 16日～ 9月 4日。利用性诱剂防治金纹细蛾效果显著 ,5个诱扑器共诱雄虫 2 584 9头。利用树干注射器注射 4 0倍速灭杀丁防治效果达 53%。     

冲击地压粘滑失稳的混沌特性

为探讨冲击地压发生的非线性特征,在分析断层型或构造型冲击地压粘滑失稳的原因和特点基础上,引入了模拟粘滑失稳的双滑块模型.理论分析表明,双滑块模型在对称情况下,完全相同的2个滑块可以造成空间上不相同的滑块运动,但其动力学行为只表现出周期性的特点;在非对称的情况下,滑块的粘滑失稳表现出复杂的混沌行为.通过适当考虑模型参数物理意义以及对参数值进行选取,该模型可用于解释断层型或构造型冲击地压粘滑失稳机理,描述其动力学行为复杂的非线性混沌特性.     

Discovery of the short gamma-ray burst GRB 050709

Gamma-ray bursts (GRBs) fall into two classes: short-hard and long-soft bursts. The latter are now known to have X-ray and optical afterglows, to occur at cosmological distances in star-forming galaxies, and to be associated with the explosion of massive stars. In contrast, the distance scale, the energy scale and the progenitors of the short bursts have remained a mystery. Here we report the discovery of a short-hard burst whose accurate localization has led to follow-up observations that have identified the X-ray afterglow and (for the first time) the optical afterglow of a short-hard burst; this in turn led to the identification of the host galaxy of the burst as a late-type galaxy at z = 0.16 (ref. 10). These results show that at least some short-hard bursts occur at cosmological distances in the outskirts of galaxies, and are likely to be caused by the merging of compact binaries.     

青檀一年生播种苗的年生长规律

青檀一年生播种苗苗高、地径的年生长变化及其地上部分生物量组分的分配模式研究结果表明,苗高、地径的生长规律符合S型生长曲线,可用Logistic方程来拟合;同时可把生长期划分为4个阶段,即出苗期（5月1日以前）、生长初期（5月1日～6月15日）、生长盛期（6月16日～8月15日）和生长后期（8月16日～10月30日）,其中、生长盛期的生长量占年生长量的60%左右。一年生播种苗地上部分各组分的生物量分配比例为叶：木质部：檀皮=40.1:47.8:12.1;苗高、地径和地上部分总生物量（檀皮）呈线性相关,且地径和地上部分总生物量及檀皮的相关系数分别要大于苗高与两的相关系数。     

Nuclear-powered millisecond pulsars and the maximum spin frequency of neutron stars

Millisecond pulsars are neutron stars that are thought to have been spun-up by mass accretion from a stellar companion. It is not known whether there is a natural brake for this process, or if it continues until the centrifugal breakup limit is reached at submillisecond periods. Many neutron stars that are accreting mass from a companion star exhibit thermonuclear X-ray bursts that last tens of seconds, caused by unstable nuclear burning on their surfaces. Millisecond-period brightness oscillations during bursts from ten neutron stars (as distinct from other rapid X-ray variability that is also observed) are thought to measure the stellar spin, but direct proof of a rotational origin has been lacking. Here we report the detection of burst oscillations at the known spin frequency of an accreting millisecond pulsar, and we show that these oscillations always have the same rotational phase. This firmly establishes burst oscillations as nuclear-powered pulsations tracing the spin of accreting neutron stars, corroborating earlier evidence. The distribution of spin frequencies of the 11 nuclear-powered pulsars cuts off well below the breakup frequency for most neutron-star models, supporting theoretical predictions that gravitational radiation losses can limit accretion torques in spinning up millisecond pulsars.     

An origin for short gamma-ray bursts unassociated with current star formation

Two short (< 2 s) gamma-ray bursts (GRBs) have recently been localized and fading afterglow counterparts detected. The combination of these two results left unclear the nature of the host galaxies of the bursts, because one was a star-forming dwarf, while the other was probably an elliptical galaxy. Here we report the X-ray localization of a short burst (GRB 050724) with unusual gamma-ray and X-ray properties. The X-ray afterglow lies off the centre of an elliptical galaxy at a redshift of z = 0.258 (ref. 5), coincident with the position determined by ground-based optical and radio observations. The low level of star formation typical for elliptical galaxies makes it unlikely that the burst originated in a supernova explosion. A supernova origin was also ruled out for GRB 050709 (refs 3, 31), even though that burst took place in a galaxy with current star formation. The isotropic energy for the short bursts is 2-3 orders of magnitude lower than that for the long bursts. Our results therefore suggest that an alternative source of bursts--the coalescence of binary systems of neutron stars or a neutron star-black hole pair--are the progenitors of short bursts.     

微尺寸单晶金属应变突变现象的随机有限元分析

微米尺寸单晶柱体的压缩实验发现,在其塑性变形过程中应变会发生突变,致使塑性流动呈现明显的间歇性. 通过随机有限元方法,分析了微米尺寸和块体镍单晶柱体在混合加载方式下的间歇性塑性流动行为. 同时,结合镍单晶柱体的实验数据以及基于经典晶体塑性理论的有限元方法,对近期新建立的理论模型进行了分析研究. 结果表明:新理论模型能够捕捉应变突变的发生;对于块体材料,新模型计算结果与常规晶体塑性有限元结果以及实验结果均比较吻合;当单晶柱体尺寸减小至几十μm左右时,新模型预测结果仍然能够与实验结果保持一致;微柱体的塑性流动是通过一系列的应变突变行为实现的.     

High-redshift galaxy populations

We now see many galaxies as they were only 800 million years after the Big Bang, and that limit may soon be exceeded when wide-field infrared detectors are widely available. Multi-wavelength studies show that there was relatively little star formation at very early times and that star formation was at its maximum at about half the age of the Universe. A small number of high-redshift objects have been found by targeting X-ray and radio sources and most recently, gamma-ray bursts. The gamma-ray burst sources may provide a way to reach even higher-redshift galaxies in the future, and to probe the first generation of stars.     

Transient radio bursts from rotating neutron stars

The radio sky is relatively unexplored for transient signals, although the potential of radio-transient searches is high. This was demonstrated recently by the discovery of a previously unknown type of source, varying on timescales of minutes to hours. Here we report a search for radio sources that vary on much shorter timescales. We found eleven objects characterized by single, dispersed bursts having durations between 2 and 30 ms. The average time intervals between bursts range from 4 min to 3 h with radio emission typically detectable for <1 s per day. From an analysis of the burst arrival times, we have identified periodicities in the range 0.4-7 s for ten of the eleven sources, suggesting origins in rotating neutron stars. Despite the small number of sources detected at present, their ephemeral nature implies a total Galactic population significantly exceeding that of the regularly pulsing radio pulsars. Five of the ten sources have periods >4 s, and the rate of change of the pulse period has been measured for three of them; for one source, we have inferred a high magnetic field strength of 5 x 10(13) G. This suggests that the new population is related to other classes of isolated neutron stars observed at X-ray and gamma-ray wavelengths.     

一种基于业务流带宽约束的前向资源预留策略

在OBS网络中，与传输路径建立时间相比，入口节点处的数据突发处理时间是影响数据突发端到端时延 的主要因素。为了减少入口节点处的数据突发时延，提出了一种基于业务流带宽约束的前向资源预留（FRR-BC） 策略。该策略使用一种新的基于业务流带宽约束的数据突发长度预测方法，以降低数据突发在入口节点处的处理 时间，同时通过业务流的带宽约束来限制数据突发的最大长度，以提高前向资源预留策略的性能。理论分析表明， 该策略使数据突发时延达到FRR的最小值。     

煤矿冲击地压事故预测控制及其动力信息系统

在深入研究我国煤矿冲击地压发生及其成功控制案例的基础上，对冲击地压事故发生的原因、灾害实现条件及其动力信息基础进行了比较系统的研究，以此为基础提出了各类冲击地压预测和控制的方法。     

一种基于业务流带宽约束的前向资源预留策略

在OBS网络中,与传输路径建立时间相比,入口节点处的数据突发处理时间是影响数据突发端到端时延的主要因素。为了减少入口节点处的数据突发时延,提出了一种基于业务流带宽约束的前向资源预留(FRR-BC)策略。该策略使用一种新的基于业务流带宽约束的数据突发长度预测方法,以降低数据突发在入口节点处的处理时间,同时通过业务流的带宽约束来限制数据突发的最大长度,以提高前向资源预留策略的性能。理论分析表明该策略使数据突发时延达到FRR的最小值。     

The afterglow of GRB 050709 and the nature of the short-hard gamma-ray bursts

The final chapter in the long-standing mystery of the gamma-ray bursts (GRBs) centres on the origin of the short-hard class of bursts, which are suspected on theoretical grounds to result from the coalescence of neutron-star or black-hole binary systems. Numerous searches for the afterglows of short-hard bursts have been made, galvanized by the revolution in our understanding of long-duration GRBs that followed the discovery in 1997 of their broadband (X-ray, optical and radio) afterglow emission. Here we present the discovery of the X-ray afterglow of a short-hard burst, GRB 050709, whose accurate position allows us to associate it unambiguously with a star-forming galaxy at redshift z = 0.160, and whose optical lightcurve definitively excludes a supernova association. Together with results from three other recent short-hard bursts, this suggests that short-hard bursts release much less energy than the long-duration GRBs. Models requiring young stellar populations, such as magnetars and collapsars, are ruled out, while coalescing degenerate binaries remain the most promising progenitor candidates.     

A gamma-ray burst with a high-energy spectral component inconsistent with the synchrotron shock model

Gamma-ray bursts are among the most powerful events in nature. These events release most of their energy as photons with energies in the range from 30 keV to a few MeV, with a smaller fraction of the energy radiated in radio, optical, and soft X-ray afterglows. The data are in general agreement with a relativistic shock model, where the prompt and afterglow emissions correspond to synchrotron radiation from shock-accelerated electrons. Here we report an observation of a high-energy (multi-MeV) spectral component in the burst of 17 October 1994 that is distinct from the previously observed lower-energy gamma-ray component. The flux of the high-energy component decays more slowly and its fluence is greater than the lower-energy component; it is described by a power law of differential photon number index approximately -1 up to about 200 MeV. This observation is difficult to explain with the standard synchrotron shock model, suggesting the presence of new phenomena such as a different non-thermal electron process, or the interaction of relativistic protons with photons at the source.     

矿井冲击地压信息识别与预报方法的研究进展

随着煤炭工业的快速发展,煤矿采深逐年加大,矿井冲击地压对煤炭工业安全生产的威胁越来越严重,研究冲击地压监测前兆信息识别与预测方法对于防治矿井自然灾害具有重要意义.对冲击地压的发生机理、传统局部监测、现代地球物理系统区域监测方法与信息识别、预报等进行了总结,展望了今后的研究热点与方向.     

由煤岩变形冲击破坏所产生的电磁辐射

对岩石破裂所产生的电磁辐射现象的观测和研究 ,对于研究地震规律和矿山冲击矿压及其预报具有重要的意义。在实验室和现场条件下 ,采用 EAE- 0 4声电测试系统和KBD5电磁辐射监测仪对煤岩变形破裂过程中的电磁辐射进行了测定。试验和测试结果表明 ,煤岩体在变形、破坏过程中均产生电磁辐射现象 ;煤岩在冲击破坏前 ,电磁辐射强度一般在某个值以下 ,而在冲击破坏时 ,电磁辐射强度突然增加 ;而电磁辐射的脉冲数则随载荷的增加及变形破裂过程的发展而增大。依此规律 ,可以对冲击矿压危险性进行评价和预测预报。