回采工作面采空区瓦斯涌出规律的数值模拟研究

从分析采空区内部的瓦斯源出发，用负指数函数描述各煤层瓦斯涌出强度的衰减过程。用迎风格式的有限元方法求解了非均质回采采空区流场的瓦斯-大气两相混溶渗流-扩散方程，以可视化技术描绘了采空区瓦斯涌出与风流交换和瓦斯分布变化规律的流体力学原理。模拟表明，采空区绝对瓦斯涌出量随工作面风量呈衰减变化。而与采空区瓦斯涌出强度呈显著地线性增加，与工作面推进度呈线性递减（但递减幅度不大）；工作面风量的突然增大会对瓦斯涌出量在短时间内（8min）产生剧烈的高峰影响，用逐渐增风方法可以避免瓦斯高峰涌出的影响。提出了采空区瓦斯涌出强度的概念，论证了用瓦斯涌出强度衡量采空区瓦斯涌出的科学意义。     

1999年度中俄合作岩石破裂实验研究

１９９９年１１月～１２月,俄罗斯科学院圣彼得堡Ｉｏｆｆｅ技术物理研究所Ｖ．Ｓ．Ｋｕｋ－ｓｅｎｋｏ教授等专家应邀来华,与中国地震局地球物理研究所和中国科学院地球物理研究所合作,在震源物理实验室开展分米级尺度岩石破裂实验研究。实验中采用了ＳＤＡＥ－８型系统,进行声发射地定位和实时显示。实验采用了多种典型构造模拟和加－卸载方式,取得了丰富的成果。该实验开辟了国际间实质性合作的新途径。     

地壳不同深度温压条件下花岗岩变形破坏及声发射时序特征.

不同深度温压条件下的三轴压缩实验结果表明,花岗岩强度随深度持续增加直至30ｋｍ左右．在地壳浅表部位,岩石破坏表现为低压突发或准突发失稳,破坏前后有分布大体均匀的声发射（acoustic emission,以下简称AE）事件发生;向下进入以渐进式破坏为特征的深度范围时,破坏前基本没有或仅有很少的、随时间逐渐稀疏的AE分布,破坏后也仅有极少的AE被记录到;在更深的以高压准突发失稳为特征的深度范围,破坏前依然AE极少,但破坏后伴随不等周期粘滑应力降的产生而有较多的AE被记录到;在更高的温压条件下（约26ｋｍ）,破坏形式为高压突发失稳,破坏前即有逐渐密集、累积频次呈指数增加的AE活动;在35ｋｍ 深度附近,岩石强度急剧降低,样品表现为半延性、延性渐进式破坏,无AE记录．声发射b值随深度增加似有减小的趋势,并且b值在岩石破坏前略小于破坏后．声发射时间序列奇异性强度因子的数值分布范围在18ｋｍ 左右深度的温压条件下最宽,表明其标度类型最多,结构最为复杂、无序;在浅部及更深部位的温压条件下均变窄．因而,当温压条件模拟真实的地壳深度向下改变时,微破裂时间序列奇异性强度因子的分布范围可能会经历由窄变宽、再由宽变窄的变化过程．      

A STUDY ON THE SOIL RESPIRATION OF THE FORESTS ON GONGGA MOUNTAIN

ＡＮＩＮＴＲＡＣＯＮＴＩＮA STUDY ON THE SOIL RESPIRATION OF THE FORESTS ON GONGGA MOUNTAINtheNational(G19980 40 80 0 )andCAS'sKeyProjectforBasicResearchonTibetanPlateau(KZ95 1 A1 2 0 4;KZ95T 0 2 )     

Optical observations of the Be/X‐ray transient system KS 1947+300

ROTSE‐IIId observations of the Be/X‐ray transient system KS 1947+300 obtained between September 2004 and December 2005 make it possible to study the correlation between optical and X‐ray activity. The optical outburst of 0.1 mag was accompanied by an increase of the X‐ray flux in the 2004 observations. A strong correlation between the optical and X‐ray light curves suggests that the neutron star directly accretes from the outflowing material of the Be star. The nearly zero time lag between X‐ray and optical light curves suggests a heating of the disk of Be star by X‐rays. No optical brightening and X‐ray enhancement was seen in the 2005 observations. There is no indication of an orbital modulation in the optical light curve. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

红外源IRAS 05437-0001和IRAS 05351+3549的CO分子谱线观测研究

利用紫金山天文台青海观测站13.7米射电望远镜对红外源IRAS05437-0001和IRAS05351+3549附近区域进行了CO(J=1-0)的分子谱线观测.发现在这两个源的方向都有很强的CO发射,CO谱线还有明显的线翼成分,这暗示两个红外源存在分子外流.同时还获得了每个源5＇×5＇的成图.通过对高速气体的空间分布的观测和分析,认为这两个源为分子外流源.其中IRAS05437-0001附近区域的外流结构比较复杂,可能这一区域的外流是多极的.IRAS05351+3549附近的外流结构较简单.从两个源的红外光谱分类以及外流的动力学时标得出都是年轻星(年龄～105yrs).通过对这两个外流源的参数估算,得出两个外流源的质量损失率.     

Electron density and temperature measurements, and abundance anomalies in the solar atmosphere

Using spectra obtained from the SUMER (Solar Ultraviolet Measurements of Emitted Radiation) spectrograph on the spacecraft SOHO (Solar and Heliospheric Observatory), we investigate the height dependence of electron density, temperature and abundance anomalies in the solar atmosphere. In particular, we present the behaviour of the solar FIP effect (the abundance enhancement of elements with first ionization potential < 10 eV in the corona with respect to photospheric values) with height above an active region observed at the solar limb, with emphasis on the so-called transition region lines.     

WR 146 – observing the OB-type companion

We present new radio and optical observations of the colliding-wind system WR 146 aimed at understanding the nature of the companion to the Wolf–Rayet (WR) star and the collision of their winds. The radio observations reveal emission from three components: the WR stellar wind, the non-thermal wind–wind interaction region and, for the first time, the stellar wind of the OB companion. This provides the unique possibility of determining the mass-loss rate and terminal wind velocity ratios of the two winds, independent of distance. Respectively, these ratios are 0.20±0.06 and 0.56±0.17 for the OB-companion star relative to the WR star. A new optical spectrum indicates that the system is more luminous than had been believed previously. We deduce that the 'companion' cannot be a single, low-luminosity O8 star as suggested previously, but is either a high-luminosity O8 star, or possibly an O8+WC binary system.     

Ammonia observations of the nearby molecular cloud MBM 12

We present NH₃(1,1) and (2,2) observations of MBM 12, the closest known molecular cloud (65-pc distance), aimed at finding evidence for on-going star formation processes. No local temperature (with a T _rot upper limit of 12 K) or linewidth enhancement is found, which suggests that the area of the cloud that we have mapped (15-arcmin size) is not currently forming stars. Therefore this nearby 'starless' molecular gas region is an ideal laboratory to study the physical conditions preceding new star formation.
A radio continuum source has been found in Very Large Array archive data, close to but outside the NH₃ emission. This source is likely to be a background object.     

Radio galaxies with a 'double-double morphology'– I. Analysis of the radio properties and evidence for interrupted activity in active galactic nuclei

We present four Mpc-sized radio galaxies which consist of a pair of double-lobed radio sources, aligned along the same axis, and with a coinciding radio core. We call these peculiar radio sources 'double-double' radio galaxies (DDRGs) and propose a general definition of such sources: a 'double-double' radio galaxy consists of a pair of double radio sources with a common centre. Furthermore, the two lobes of the inner radio source must have a clearly extended, edge-brightened radio morphology. Adopting this definition, we find several other candidate DDRGs in the literature. We find that in all sources the smaller (inner) pair of radio lobes is less luminous than the larger (outer) pair, and that the ratio of 1.4-GHz flux density of these two pairs appears to be anticorrelated with the projected linear size of the inner source. Also, the outer radio structures are large, exceeding 700 kpc. We discuss possible formation scenarios of the DDRGs, and we conclude that an interruption of the jet-forming central activity is the most likely mechanism. For one of our sources (B 1834+620) we have been able observationally to constrain the length of time of the interruption to a few Myr. We discuss several scenarios for the cause of the interruption, and suggest multiple encounters between interacting galaxies as a possibility. Finally, we discuss whether such interruptions help the formation of extremely large radio sources.