灾后重建要加强区域地壳稳定性评价

<正>距汶川特大地震还不到两年,玉树又发生了7.1级地震。与汶川特大地震相比,玉树的震级尽管低一些,但造成的地质灾害、人员伤亡却相当严重。玉树地震诱发的地质灾害主要有四个特点,即:低位土质滑坡很多、高位山体稳     

1∶25万常德市幅构造-沉积地貌类型划分及其对江汉—洞庭盆地第四纪地质与环境研究的启示

1:25万常德市幅自西向东跨武陵隆起和江汉—洞庭盆地,具复杂的第四纪隆-凹构造格局。以详细地表调查和大量第四系钻孔资料为基础,以第四纪构造活动、沉积作用以及现今地势高低和地貌形态特征为主要依据,对1∶25万常德市幅进行了构造-沉积地貌类型的划分与编图。构造-沉积地貌类型是以第四纪地质作用为依据对传统地貌类型和地貌单元所作的分解和细化。研究区共厘定出抬升剥蚀中低山(Ⅰ)、抬升剥蚀丘陵(Ⅱ)、沉积-抬蚀丘陵(Ⅲ)、沉积-抬蚀岗状平原(Ⅳ)、残坡积岗状平原(Ⅴ)、孤山(Ⅵ)、沉降沉积-抬蚀岗状平原(Ⅶ)、沉降沉积-抬升波状平原(Ⅷ)、稳定沉积低平原(Ⅸ)、沉降沉积低平原(Ⅹ)等10种构造-沉积地貌类型。详细的解析表明,不同构造-沉积地貌类型的地表高程、第四纪地壳升降特征、风化剥蚀和沉积作用等各具特征。构造-沉积地貌类型的划分及其地貌图的编制,不仅反映出地表地理环境暨地貌特征,同时提供了直观表达不同地区第四纪地层、构造特征及其反映的地质与环境演化过程的有效途径,有助于促进和深化江汉-洞庭盆地第四纪地质与环境研究。     

Relationship between CME dynamics and solar flare plasma

The relationship between the velocity of CMEs and the plasma temperature of the associated X-ray solar flares is investigated.The velocity of CMEs increases with plasma temperature(R=0.82)and photon index below the break energy(R=0.60)of X-ray flares.The heating of the coronal plasma appears to be significant with respect to the kinetics of a CME from the reconnection region where the flare also occurs.We propose that the initiation and velocity of CMEs perhaps depend upon the dominant process of conversion of the magnetic field energy of the active region to heating/accelerating the coronal plasma in the reconnected loops.Results show that a flare and the associated CME are two components of one energy release system,perhaps,magnetic field free energy.     

Propagation of a strong cylindrical shock wave in a rotational axisymmetric dusty gas with exponentially varying density

Non-similarity solutions are obtained for one-dimensional isothermal and adiabatic flow behind strong cylindrical shock wave propagation in a rotational axisymmetric dusty gas,which has a variable azimuthal and axial fluid velocity.The dusty gas is assumed to be a mixture of small solid particles and perfect gas.The equilibrium flow conditions are assumed to be maintained,and the density of the mixture is assumed to be varying and obeying an exponential law.The fluid velocities in the ambient medium are assumed to obey exponential laws.The shock wave moves with variable velocity.The effects of variation of the mass concentration of solid particles in the mixture,and the ratio of the density of solid particles to the initial density of the gas on the flow variables in the region behind the shock are investigated at given times.Also,a comparison between the solutions in the cases of isothermal and adiabatic flows is made.     

A new three-stage evolution model for millimeter to centimeter wavelength outbursts in BL Lacertae

The multi-frequency light curves of BL Lacertae during 1997.5 – 1999.5 have been modeled by four outbursts,each having a 3-stage evolution in the (S m,νm) plane with distinct rising–plateau–decaying phases.It is shown that the observed light curves can be well fitted for the eight frequencies from 350GHz to 4.8GHz.The main characteristics of the model-fitting are: (1) the outbursts are found to have very flat spectra with an optically thin spectral index α (defined as Sν∝ν-α) of about 0.15.This is consisten...     

暗物质晕次结构的演化研究进展

一般认为暗晕是通过等级成团方式形成的:小质量暗晕先形成,进而通过并合形成较大质量的暗晕。并合后的小质量暗晕形成所谓的次结构,目前关于次结构的演化过程和分布特点尚无明确结论。介绍了利用数值模拟、半解析模型和观测来研究次结构分布和演化的进展,并特别讨论了次结构的并合时标、质量函数和空间分布等特性。     

活动星系核射电延展区观测和理论研究

随着探测设备角分辨率和灵敏度的提高,喷流、喷流节点和热斑等活动星系核延展结构在射电、红外、光学、X射线等越来越多的波段被探测到,分辨出其更细致的结构,促进了理论研究热潮的兴起,使该领域成为当今天体物理研究的活跃领域之一。喷流是由活动星系核中心产生的准直等离子体外流,由中心黑洞驱动。至今,对喷流的成分、产生、准直原理和加速机制等基本问题并不清楚。另一方面,对于喷流、喷流节点和热斑等活动星系核延展区的辐射机制,一般认为其射电和光学辐射由相对论电子的同步辐射产生,但X射线的起源就存在着一定的争议。简单概述该领域近年来观测和理论研究进展。     

The Filament Eruption of 1999 March 21 and Its Associated Coronal Dimmings and CME

We report a filament eruption near the center of the solar disk on 1999 March 21, in multi-wavelength observations by the Yohkoh Soft X-Ray Telescope (SXT), the Extreme-ultraviolet Images Telescope (EIT) and the Michelson Doppler Imager (MDI) on the Solar and Heliospheric Observatory (SOHO). The eruption involved in the disappearance of an Ha filament can be clearly identified in EIT 195 A difference images. Two flare-like EUV ribbons and two obvious coronal dimming regions were formed. The two dimming regions had a similar appearance in lines formed in temperature range 6×104 K to several 106 K. They were located in regions of opposite magnetic polarities near the two ends of the eruptive filament. No significant X-ray or Ha flare was recorded associated with the eruption and no obvious photospheric magnetic activity was detected around the eruptive region, and particularly below the coronal dimming regions. The above surface activities were closely associated with a partial halo-type coronal mass ejection (CME) observed by the Large Angle and Spectrometric Coronagraphs (LASCO) on the SOHO. In terms of the magnetic flux rope model of CMEs, we explained these multiple observations as an integral process of large-scale rearrangement of coronal magnetic field initiated by the filament eruption, in which the dimming regions marked the evacuated feet of the flux rope.     

The Relation between the Inclinations of Broad Line Regions and the Accretion Disk

According to the standard model, an active galactic nucleus (AGN) consists of an inner accretion disk with a jet around a central massive black hole, and a number of outer broad line regions (BLRs) and narrow line regions (NLRs). The geometrical relationship between the BLRs and the accretion disk is not well understood. Assuming the motion of the BLRs is virialized and its configuration is disk-like, we derived its inclination to the line of sight for a sample of AGNs from their bulge stellar velocity dispersion, their size of the BLRs and their Hβ linewidth. Compared with the inclination of the accretion disk obtained from the X-ray Fe Kα emission lines, we found that there is no positive correlation between the two. Our results showed that BLRs are not coplanar with the accretion disk and that we should be cautious of using the BLRs inclination as the disk inclination. The non-coplanar geometry of the outer BLRs and the inner accretion disk provides clues to the origin of BLRs and the properties of the accretion disk. Our preferable interpretation is that BLRs arise out of the outer part of a warped accretion disk.