考虑时程竖向加速度的Newmark滑块位移法   总被引：2，自引：1，他引：1  

李红军  迟世春  钟红  林皋 《岩土力学》2007,28(11):2385-2390

利用改进的Newmark滑块位移法,采用时程竖向加速度计算屈服角加速度,运用拟静力极限平衡分析和地震动力反应分析计算土工结构地震永久变形。算例计算结果表明,屈服角加速度计算采用时程竖向加速度得到的滑动位移位于竖向加速度假定恒定向上或向下之间。适当改变筑坝土石料的动力刚度,研究了滑动体位移关于动力刚度的敏感性,为土工建筑物的抗震设计提供依据。  相似文献   

粗粒土组构之颗粒运动研究     

程展林  吴良平  丁红顺 《岩土力学》2007,28(Z1):29-33

土的结构性是决定土的力学特性的一个最根本的因素,正是由于土的结构性的存在,连续体力学理论用于岩土材料存在明显不足,沈珠江将土体结构性的研究提到“21世纪土力学的核心问题”的高度,但由于土的结构性的复杂性,缺乏测试方法,还没有找到土结构性的定量指标。选择结构特征相对简单的粗粒土作为研究对象,探索建立其力学体系的方法和途径。粗粒土的结构性（称之为组构）主要体现在颗粒的排列特征方面,采用CT测试技术和DDA数值分析方法初步解决了粗粒土组构的量化问题,对粗粒土多种受力过程进行了CT三轴试验和数值模拟,取得了粗粒土的组构信息及其变化,为构成合理的组构量、研究粗粒土组构量与宏观力学响应之间的相互关系、探讨粗粒土的变形机理和力学特征奠定了基础,并侧重介绍粗粒土CT三轴试验成果,展示三轴试验过程中颗粒运动规律。  相似文献   

高温下混凝土水力、热及变形耦合数学模型     

沈新普  沈国晓  刘继行 《岩土力学》2007,28(Z1):137-143

针对受高温载荷的混凝土提出了一个水力-热-变形耦合的数学模型,模型中采用了3种不同的连续介质：水蒸汽与干燥空气的混合气体相,液态水以及固态混凝土骨架。在连续介质的Navier-Stokes方程基础上,推导了各相介质的质量守恒方程、动量守恒方程以及混合物整体的能量守恒方程。为了简化问题,引入了若干假设,给出了基于文献资料数据拟合的某些变量的用基本未知量表达的经验公式,建立了基于物理定律的各类运动学变量与其热力学共轭力的本构关系,并给出了系统偏微分方程。  相似文献   

青藏高原东北部新构造运动特征   总被引：2，自引：0，他引：2  

刘高  聂德新张斌 《山地学报》2000,18(Z1):30-33

用大陆动力学和岩石圈动力学理论,讨论了青藏高原东北部的新构造运动特征,并探讨了这些特征的根本原因。  相似文献   

WR 146 – observing the OB-type companion     

S. M. Dougherty  P. M. Williams  D. L. Pollacco 《Monthly notices of the Royal Astronomical Society》2000,316(1):143-151

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.  相似文献   

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

Arno P. Schoenmakers  †  A. G. de Bruyn  H. J. A. Röttgering  H. van der Laan  C. R. Kaiser 《Monthly notices of the Royal Astronomical Society》2000,315(2):371-380

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.  相似文献   

Non-thermal emission in Wolf–Rayet stars: are massive companions required?     

S. M. Dougherty  P. M. Williams 《Monthly notices of the Royal Astronomical Society》2000,319(4):1005-1010

We examine the radio spectral indices of 23 Wolf–Rayet (WR) stars to identify the nature of their radio emission. We identify nine systems as non-thermal emitters. In seven of these systems the non-thermal emission dominates the radio spectrum, while in the remaining two it is of comparable strength to the thermal, stellar wind emission, giving 'composite' spectra. Among these nine systems, seven have known spectroscopic or visual binary companions. The companions are all massive O or early B-type stars, strongly supporting a connection between the appearance of non-thermal emission in WR stars and the presence of a massive companion. In three of these binaries, the origin of non-thermal emission in a wind-collision region between the stars has been well established in earlier work. The binary systems that exhibit only thermal emission are all short‐period systems where a wind-collision zone is deep within the opaque region of the stellar wind of the WR star. To detect non-thermal emission in these systems requires optically thin lines of sight to the wind-collision region.  相似文献   

Analysis of λ = 6 cm VLBI polarization observations of a complete sample of northern BL Lacertae objects     

D. C. Gabuzda  A. B. Pushkarev  T. V. Cawthorne 《Monthly notices of the Royal Astronomical Society》2000,319(4):1109-1124

The results of very long baseline interferometry (VLBI) total intensity ( I ) and linear polarization ( P ) observations at     are presented for 10 radio bright BL Lacertae objects. These images complete first-epoch polarization observations for the 1-Jy sample of northern BL Lacertae objects defined by Kühr & Schmidt. Estimates of superluminal speeds are presented for several sources, bringing the total number of sources in the sample for which such estimates are available to 16. Second-epoch observations currently being reduced should yield speed estimates for VLBI features in essentially all the sources in the sample. The jet magnetic fields of these BL Lacertae objects are usually transverse to the local jet direction, but a sizeable minority (about 30 per cent) have VLBI jet components with longitudinal magnetic fields. This may suggest that the conditions in the VLBI jets of BL Lacertae objects are favourable for the formation of relativistic shocks; alternatively, it may be that the toroidal component of the intrinsic jet magnetic field is characteristically dominant in these sources.  相似文献   

The remnant of Nova Cassiopeiae 1993 (V705 Cassiopeiae)     

S. P. S. Eyres  M. F. Bode  T. J. O'Brien  S. K. Watson  R. J. Davis 《Monthly notices of the Royal Astronomical Society》2000,318(4):1086-1092

We have detected radio emission from the remnant of V705 Cas, beginning 221 d after visual maximum. We follow the remnant from first detection while still optically thick through the turn-over to optically thin emission, and finally confirming the absence of emission due to expansion and fading by the end of 1998. While the emission is consistent with thermal bremsstrahlung, as seen in most previous novae, the small-scale structure shows two ridge-like features, which develop significantly from day 585 until our last detection on day 1544. While the development is fairly rapid, it is also much smoother than that seen in V1974 Cyg, in that we can follow individual features as they change over almost 1000 d. Our optical spectra unequivocally indicate some form of axial symmetry, as derived from the velocity structure. This is difficult to reconcile with the observed development in the radio images. We suggest a number of possible explanations.  相似文献   

The very flat radio–millimetre spectrum of Cygnus X-1     

R. P. Fender  G. G. Pooley  P. Durouchoux  R. P. J. Tilanus  C. Brocksopp 《Monthly notices of the Royal Astronomical Society》2000,312(4):853-858

We present almost-simultaneous detections of Cygnus X-1 in the radio and mm regimes, obtained during the low/hard X-ray state. The source displays a flat spectrum between 2 and 220 GHz, with a spectral index | α |0.15 (3 σ ). There is no evidence for either a low- or high-frequency cut-off, but in the mid-infrared (∼30 μm) thermal emission from the OB-type companion star becomes dominant. The integrated luminosity of this flat-spectrum emission in quiescence is 2×10³¹ erg s⁻¹ (2×10²⁴ W). Assuming the emission originates in a jet for which non-radiative (e.g. adiabatic expansion) losses dominate, this is a very conservative lower limit on the power required to maintain the jet. A comparison with Cyg X-3 and GRS 1915+105, the other X-ray binaries for which a flat spectrum at shorter than cm wavelengths has been observed, shows that the jet in Cyg X-1 is significantly less luminous and less variable, and is probably our best example to date of a continuous, steady, outflow from an X-ray binary. The emissive mechanism responsible for such a flat spectral component remains uncertain. Specifically, we note that the radio–mm spectra observed from these X-ray binaries are much flatter than those of the 'flat-spectrum' AGN, and that existing models of synchrotron emission from partially self-absorbed radio cores, which predict a high-frequency cut-off in the mm regime, are not directly applicable.  相似文献