Eliminating Virtual Impactors with the Very Large Telescope: An ESO Program with the FORS2 Camera     

A.?BoattiniEmail author  G.?D’Abramo  H.?Scholl  O.?R.?Hainaut  R.?West  G.?Hahn  R.?Michelsen  G.?Forti  P.?Pravec  G.?B.?Valsecchi 《Earth, Moon, and Planets》2003,93(4):239-248

We have used the ESO Very Large Telescope (VLT) to perform as trometric observations of Near Earth Asteroids (NEAs) having remote collision possibilities with the Earth. The observations were made for those objects which became too faint to be observed elsewhere. Using the 4 hours allocated in the semester April–September 2003, 5 faint NEAs were observed. As a result, no NEA that could impact the Earth was lost.  相似文献   

温度对土壤水分运动影响的研究进展   总被引：10，自引：0，他引：10       下载免费PDF全文

冯宝平  张展羽  张建丰  汪志荣 《水科学进展》2002,13(5):643-648

综述了温度对土壤水分运动的影响,温度影响的机理和考虑温度影响的土壤水分运动的数学模型,以及目前所用的实验研究方法,同时提出了本领域中存在的主要问题及研究展望.  相似文献   

Evolution of Planetesimal Velocities Based on Three-Body Orbital Integrations and Growth of Protoplanets     

Keiji OhtsukiGlen R. Stewart  Shigeru Ida 《Icarus》2002,155(2):436-453

We obtain the viscous stirring and dynamical friction rates of planetesimals with a Rayleigh distribution of eccentricities and inclinations, using three-body orbital integration and the procedure described by Ohtsuki (1999, Icarus137, 152), who evaluated these rates for ring particles. We find that these rates based on orbital integrations agree quite well with the analytic results of Stewart and Ida (2000, Icarus 143, 28) in high-velocity cases. In low-velocity cases where Kepler shear dominates the relative velocity, however, the three-body calculations show significant deviation from the formulas of Stewart and Ida, who did not investigate the rates for low velocities in detail but just presented a simple interpolation formula between their high-velocity formula and the numerical results for circular orbits. We calculate evolution of root mean square eccentricities and inclinations using the above stirring rates based on orbital integrations, and find excellent agreement with N-body simulations for both one- and two-component systems, even in the low-velocity cases. We derive semi-analytic formulas for the stirring and dynamical friction rates based on our numerical results, and confirm that they reproduce the results of N-body simulations with sufficient accuracy. Using these formulas, we calculate equilibrium velocities of planetesimals with given size distributions. At a stage before the onset of runaway growth of large bodies, the velocity distribution calculated by our new formulas are found to agree quite well with those obtained by using the formulas of Stewart and Ida or Wetherill and Stewart (1993, Icarus106, 190). However, at later stages, we find that the inclinations of small collisional fragments calculated by our new formulas can be much smaller than those calculated by the previously obtained formulas, so that they are more easily accreted by larger bodies in our case. The results essentially support the previous results such as runaway growth of protoplanets, but they could enhance their growth rate by 10-30% after early runaway growth, where those fragments with low random velocities can significantly contribute to rapid growth of runaway bodies.  相似文献   

Can origin of the 2400-year cycle of solar activity be caused by solar inertial motion?     

I. Charvátová 《Annales Geophysicae》2000,18(4):399-405

A solar activity cycle of about 2400 years has until now been of uncertain origin. Recent results indicate it is caused by solar inertial motion. First we describe the 178.7-year basic cycle of solar motion. The longer cycle, over an 8000 year interval, is found to average 2402.2 years. This corresponds to the Jupiter/Heliocentre/Barycentre alignments (9.8855 × 243). Within each cycle an exceptional segment of 370 years has been found characterized by a looping pattern by a trefoil or quasitrefoil geometry. Solar activity, evidenced by ¹⁴C tree-ring proxies, shows the same pattern. Solar motion is computable in advance, so this provides a basis for future predictive assessments. The next 370-year segment will occur between AD 2240 and 2610.  相似文献   

地形对水平岩层自重成因地应力场的影响     

陶波  伍法权  郭改梅 《煤田地质与勘探》2006,34(1):34-37

通过极坐标系下的艾里应力函数法,求解出在集中力作用下水平岩层中各应力分量。山体对其下伏岩层可作为分布载荷,对集中力作用下水平岩层中各应力分量积分,便求得山体对下伏水平岩层的附加应力。已有研究成果表明,当由外载引起的附加应力小于由重力引起的静止侧压力的20%时,则可以不考虑外载的影响,这样便导出了地形对自重应力影响深度所满足的函数关系式。此外,本文举例说明了如何求得地形对水平均质各向同性水平岩层的自重应力场的影响深度。  相似文献   

Can Damage Mechanics Explain Temporal Scaling Laws in Brittle Fracture and Seismicity?     

Donald L. Turcotte  Robert Shcherbakov 《Pure and Applied Geophysics》2006,163(5-6):1031-1045

Time delays associated with processes leading to a failure or stress relaxation in materials and earthquakes are studied in terms of continuum damage mechanics. Damage mechanics is a quasi-empirical approach that describes inelastic irreversible phenomena in the deformation of solids. When a rock sample is loaded, there is generally a time delay before the rock fails. This period is characterized by the occurrence and coalescence of microcracks which radiate acoustic signals of broad amplitudes. These acoustic emission events have been shown to exhibit power-law scaling as they increase in intensity prior to a rupture. In case of seismogenic processes in the Earth's brittle crust, all earthquakes are followed by an aftershock sequence. A universal feature of aftershocks is that their rate decays in time according to the modified Omori's law, a power-law decay. In this paper a model of continuum damage mechanics in which damage (microcracking) starts to develop when the applied stress exceeds a prescribed yield stress (a material parameter) is introduced to explain both laboratory experiments and systematic temporal variations in seismicity.  相似文献   

碎石土地基湿陷性研究   总被引：1，自引：0，他引：1  

张管宏  谌文武  王生新 《岩土工程技术》2006,20(3):136-139

主要以甘南330 kV变电所碎石土地基的现场浸水载荷试验和室内实验为基础,根据湿陷变形的特征,分析了影响碎石土地基湿陷变形的主要影响因素,探讨了碎石土地基的湿陷机理。认为碎石等大骨架颗粒与细粒胶结物相填充的特殊结构是碎石土地基湿陷最主要的原因。碎石土由于浸水骨架颗粒之间抗剪、抗压强度降低而导致碎石土结构破坏,随之填充在骨架颗粒之间的细颗粒产生二次湿陷,两者引起土体体积减小所导致。  相似文献   

非饱和土土水特征曲线(SWCC)测试与预测   总被引：3，自引：0，他引：3  

李志清  李涛  胡瑞林  李熊  李壮举 《工程地质学报》2007,15(5):700-707

非饱和土土水特征曲线(SWCC)表示了土中含水量与吸力之间的关系。文章介绍了6种常用方法,各有其适用范围。体积压力板仪可量测最大基质吸力值为1500kPa的干燥曲线和浸湿曲线;超过1500kPa时,可用盐溶液法进行量测;Tem-ple仪可量测基质吸力达100kPa的干燥曲线;滤纸法可用于测量土体的基质吸力与总吸力;Dew-point电位计可用于量测土样总吸力变化,尤其适合渗透吸力的量测;TDR探头适合于量测小于300kPa的基质吸力。用GDS非饱和土三轴仪可以进行SWCC测试,测试范围主要取决于陶土板的进气值。用准确的数学模型对测得的含水量、吸力数据进行拟合,对于预测非饱和土力学性质、渗透系数、抗剪强度及分析边坡稳定性有重要意义。由于准确测试SWCC难度较大,并且测试影响因素较多,所以根据土体孔隙大小分布和颗粒大小分布情况预测SWCC,也是一种较好的方法。  相似文献   

气候影响下膨胀土开裂的力学分析   总被引：1，自引：0，他引：1  

郑少河  姚海林  葛修润 《上海国土资源》2007,(2):29-32

采用线弹性断裂力学的方法,针对气候影响下的膨胀土开裂问题,提出了膨胀土开裂深度和裂缝间距的定量表达式,经比较与现场实测结果基本一致。并对开裂深度与泊松比、断裂韧度、基质吸力等土体特性参数的关系进行了详细的论述。  相似文献   

On the Dynamics of Dust Grains in a Hierarchical Environment     

Marcos  C. De La Fuente  Marcos  R. De La Fuente 《Earth, Moon, and Planets》1998,81(2):145-173

Most main sequence stars are binaries or higher multiplicity Systems and it appears that at birth most stars have circumstellar disks. It is commonly accepted that planetary systems arise from the material of these disks; consequently, binary and multiple systems may have a main role in planet formation. In this paper, we study the stage of planetary formation during which the particulate material is still dispersed as centimetre-to-metre sized primordial aggregates. We investigate the response of the particles, in a protoplanetary disk with radius R_D = 100 AU around a solar-like star, to the gravitational field of bound perturbing companions in a moderately wide (300–1600 AU) orbit. For this purpose, we have carried out a series of simulations of coplanar hierarchical configurations using a direct integration code that models gravitational and viscous forces. The massive protoplanetary disk is around one of the components of the binary. The evolution in time of the dust sub-disk depends mainly on the nature (prograde or retrograde) of the relative revolution of the stellar companion, and on the temperature and mass of the circumstellar disk. Our results show that for binary companions near the limit of tidal truncation of the disk, the perturbation leads to an enhanced accretion rate onto the primary, decreasing the lifetime of the particles in the protoplanetary disk with respect to the case of a single star. As a consequence of an enhanced accretion rate the mass of the disk decreases faster, which leads to a longer resultant lifetime for particles in the disk. On the other hand, binary companions may induce tidal arms in the dust phase of protoplanetary disks. Spiral perturbations with m = 1 may increase in a factor 10 or more the dust surface density in the neighbourhood of the arm, facilitating the growth of the particles. Moreover, in a massive disk (0.01M⊙) the survival time of particles is significantly shorter than in a less massive nebula (0.001M⊙) and the temperature of the disk severely influences the spiral-in time of particles. The rapid evolution of the dust component found in post T Tauri stars can be explained as a result of their binary nature. Binarity may also influence the evolution of circumpulsar disks. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献