重大工程建设中的地应力测量及其在设计中的应用

水压致裂技术现已发展成为确定地下洞室三维原地应力状态、高压洞室围岩的自身承载能力以及岩体高压透水性的可靠实用方法,并已经在核废料处置、长大深埋交通隧道以及水电站高压力洞室工程中得到广泛应用。实践表明,综合测定岩体的物理力学参数,充分利用围岩承载力优化工程设计,对确保工程安全和提高设计水平具有重要意义。     

Photometric Observation And Period Study Of Go Cygni

Photometric observations of GO Cyg were performed during July–October 2002, in B and V filters (Johnson system). Using the Wilson's computer codes, the light curve analysis were carried out to find the photometric elements of the system. The O-C diagram which is based on the observed times of minima as well as those found in the literature, suggests a negative rate of period variation (i.e. ) for the system.     

塔克拉玛干沙漠腹地沙尘气溶胶质量浓度垂直分布特征

 利用Grimm 1.108、Thermo RP 1 400 a以及TSP等仪器于2009年1月至2010年2月对塔克拉玛干沙漠腹地塔中不同高度沙尘气溶胶质量浓度进行连续观测,结合天气资料进行分析。结果表明:①80 m高度PM10质量浓度最高,80 m高度PM2.5和PM1.0质量浓度明显低于4 m高度PM10,80 m高度PM1.0质量浓度最低。频繁的沙尘天气是影响不同粒径的沙尘气溶胶浓度含量的主要因素。②夜间至日出,PM质量浓度逐渐降低,最低基本上出现在08:00,随后质量浓度逐渐增大,18:00前后浓度达到最高值,然后又逐步降低。其规律与风速的昼夜变化完全一致。③TSP月平均质量浓度高值主要集中在3—9月,其中4月和5月浓度最高,随后逐渐减低。3—9月也是PM月平均质量浓度的高值区域,4 m高度PM10月平均质量浓度最高发生在5月,其浓度为846.0 μg·m-3。80 m高度PM10浓度远高于PM2.5和PM1.0浓度,PM2.5和PM1.0浓度相差较小。风沙天气对大气中的不同粒径粒子的浓度含量影响较大,风沙天气越多,粗颗粒含量越高,反之则细颗粒越多。④沙尘天气过程中不同粒径沙尘气溶胶质量浓度变化具有晴天<浮尘天气<扬沙天气<沙尘暴天气的规律。各种沙尘天气中,PM10/TSP表现为晴好天气高于浮尘天气,浮尘天气远高于扬沙和沙尘暴天气。⑤沙尘天气过程中,沙尘气溶胶浓度随着粒径的减小,浓度逐渐降低。不同高度、不同粒径的沙尘气溶胶质量浓度每隔3~4 d形成一个峰值区,与每隔3~4 d出现沙尘天气强度增强过程直接相关。     

山体效应及其对林线分布的影响(英文)

The concept of mass elevation effect(massenerhebungseffect,MEE) was intro-duced by A.de Quervain about 100 years ago to account for the observed tendency for temperature-related parameters such as tree line and snowline to occur at higher elevations in the central Alps than on their outer margins.It also has been widely observed in other ar-eas of the world,but there have not been significant,let alone quantitative,researches on this phenomenon.Especially,it has been usually completely neglected in developing fitting mod-els of timberline elevation,with only longitude or latitude considered as impacting factors.This paper tries to quantify the contribution of MEE to timberline elevation.Considering that the more extensive the land mass and especially the higher the mountain base in the interior of land mass,the greater the mass elevation effect,this paper takes mountain base elevation(MBE) as the magnitude of MEE.We collect 157 data points of timberline elevation,and use their latitude,longitude and MBE as independent variables to build a multiple linear regres-sion equation for timberline elevation in the southeastern Eurasian continent.The results turn out that the contribution of latitude,longitude and MBE to timberline altitude reach 25.11%,29.43%,and 45.46%,respectively.North of northern latitude 32°,the three factors’ contribu-tion amount to 48.50%,24.04%,and 27.46%,respectively;to the south,their contribution is 13.01%,48.33%,and 38.66%,respectively.This means that MBE,serving as a proxy indi-cator of MEE,is a significant factor determining the elevation of alpine timberline.Compared with other factors,it is more stable and independent in affecting timberline elevation.Of course,the magnitude of the actual MEE is certainly determined by other factors,including mountain area and height,the distance to the edge of a land mass,the structures of the mountains nearby.These factors need to be included in the study of MEE quantification in the future.This paper could help build up a high-accuracy and multi-scale elevation model for alpine timberline and even other altitudinal belts.     

Using X-ray observations to explore the binary interaction in Eta Carinae

We study the usage of the X-ray light curve, column density towards the hard X-ray source, and emission measure (density square times volume), of the massive binary system η Carinae to determine the orientation of its semimajor axis. The source of the hard X-ray emission is the shocked secondary wind. We argue that, by itself, the observed X-ray flux cannot teach us much about the orientation of the semimajor axis. Minor adjustment of some unknown parameters of the binary system allows to fit the X-ray light curve with almost any inclination angle and orientation. The column density and X-ray emission measure, on the other hand, impose strong constrains on the orientation. We improve our previous calculations and show that the column density is more compatible with an orientation where for most of the time the secondary – the hotter, less massive star – is behind the primary star. The secondary comes closer to the observer only for a short time near periastron passage. The 10-week X-ray deep minimum, which results from a large decrease in the emission measure, implies that the regular secondary wind is substantially suppressed during that period. This suppression is most likely resulted by accretion of mass from the dense wind of the primary luminous blue variable star. The accretion from the equatorial plane might lead to the formation of a polar outflow. We suggest that the polar outflow contributes to the soft X-ray emission during the X-ray minimum; the other source is the shocked secondary wind in the tail. The conclusion that accretion occurs at each periastron passage, every five and a half years, implies that accretion had occurred at a much higher rate during the Great Eruption of η Car in the 19th century. This has far reaching implications for major eruptions of luminous blue variable stars.     

Acceleration of Relativistic Protons During the 20 January 2005 Flare and CME

The origin of relativistic solar protons during large flare/CME events has not been uniquely identified so far. We perform a detailed comparative analysis of the time profiles of relativistic protons detected by the worldwide network of neutron monitors at Earth with electromagnetic signatures of particle acceleration in the solar corona during the large particle event of 20 January 2005. The intensity – time profile of the relativistic protons derived from the neutron monitor data indicates two successive peaks. We show that microwave, hard X-ray, and γ-ray emissions display several episodes of particle acceleration within the impulsive flare phase. The first relativistic protons detected at Earth are accelerated together with relativistic electrons and with protons that produce pion-decay γ rays during the second episode. The second peak in the relativistic proton profile at Earth is accompanied by new signatures of particle acceleration in the corona within ≈1R _⊙ above the photosphere, revealed by hard X-ray and microwave emissions of low intensity and by the renewed radio emission of electron beams and of a coronal shock wave. We discuss the observations in terms of different scenarios of particle acceleration in the corona.     

Why Do Temperature and Velocity Have Different Relationships in the Solar Wind and in Interplanetary Coronal Mass Ejections?

In-situ observations of the solar wind (SW) show temperature increasing with the wind speed, whereas such a dependence is not observed in interplanetary coronal mass ejections (ICMEs). The aim of this paper is to understand the main origin of this correlation in the SW and its absence in ICMEs. For that purpose both the internal-energy and momentum equations are solved analytically with various approximations. The internal-energy equation does not provide a strong link between temperature and velocity, but the momentum equation does. Indeed, the observed correlation in the open magnetic-field configuration of the SW is the result of its acceleration and heating close to the Sun. In contrast, the magnetic configuration of ICMEs is closed, and moreover the momentum equation is dominated by magnetic forces. This implies no significant correlation between temperature and velocity, as observed.     

Possible dark matter in spiral galaxies of the coma cluster

The relationship between the rotation curves for the galaxies and the distribution of mass and angular momentum within the galaxies is examined. The theory of angular momentum transfer is applied to the observed properties of the galaxies. The coupling between the dynamical mass of a spiral galaxy and its luminosity is studied. Most of the spiral galaxies in subclusters surrounding NGC 4889, NGC 4874, and NGC 4839 in the Coma cluster are galaxies that have lower luminosities, with M_B fainter than −21^m.5. These galaxies are characterized by a higher mass-to-luminosity ratio than that of the galaxies with higher luminosities M_B brighter than −21^m.5, which suggests the presence of a large fraction of dark matter in the spiral galaxies of the subclusters. Translated from Astrofizika, Vol. 52, No. 1, pp. 75–84 (February 2009).