Theoretical Derivation of a Peak Particle Velocity–Distance Law for the Prediction of Vibrations from Blasting

I would like to suggest a theoretical justification for the mathematical structure of some laws for predicting the maximum particle velocity vibration from blasting operations in the light of some basic notions of elastic and anelastic wave theory. Within this point of view, in dimensionally correct expressions, the terms pertaining to the rock, to the blast and to the seismic wave become evident and recognisable. A law is presented that can be used to forecast the maximum particle velocity on the basis of some blast design and rock parameters. Four tests of the proposed law performed with real data sets seem to confirm fairly well its reliability.     

Dark energy and the anthropic principle

The Hubble constant is split into two terms H = H₁ + H₂ , where H₁ is a decreasing function due to the Big Bang and the subsequent gravitational interaction that slows the expansion of the Universe and H₂ is an increasing function that corresponds to dark energy which accelerates this expansion. For T = 13.7 Gyr we prove that H₂(T) > 5 m/(yr AU). This is a quite large number and thus the impact of dark energy, which is spread almost everywhere uniformly, should be observable not only on large scales, but also in our Solar system. In particular, we show that Earth, Mars and other planets were closer to the Sun 4.5 Gyr ago. The recession speed ≈5.3 m/yr of the Earth from the Sun seems to be just right for an almost constant influx of solar energy from the origin of life on Earth up to the present over which time the Sun’s luminosity has increased approximately linearly. This presents further support for the Anthropic Principle. Namely, the existence of dark energy guarantees very stable conditions for the development of intelligent life on Earth over a period of 3.5 Gyr.     

A modified Raupach's model applicable for shear-stress partitioning on surfaces covered with dense and flat-shaped gravel roughness elements

A commonly used measure to prevent soil wind erosion is to cover the surface with gravel. Gravel can inhibit soil erosion by covering the surface directly, changing the airflow field near the surface and sharing the shear stress of wind. Similar to other roughness elements, the protective effect of gravel on soil is usually expressed in terms of the ratio of the shear stress on the exposed soil surface to the total shear stress on the rough surface due to wind, i.e. through a shear-stress partitioning model. However, the existing shear-stress partitioning models, represented by Raupach's model (RM93), are only applicable when the lateral coverage of the roughness elements, λ < 0.10, and the applicability of the models to flat-shaped roughness elements is unclear. The purpose of this study is to verify the applicability of RM93 for dense and flat-shaped gravel roughness elements by using shear-stress data from wind-tunnel measurements pertaining to roughness elements with different densities (0.013 ≤ λ ≤ 0.318) and flat shapes (height-to-width ratios in the range 0.20 ≤ H/W ≤ 0.63), and to modify RM93 to enhance its predictive ability. The results indicate that RM93 cannot accurately predict the shear-stress partitioning for surfaces covered by densely distributed and flat-shaped gravel roughness elements. This phenomenon occurs because, when roughness elements are distributed densely or are flat-shaped, the proportion of the shear stress on the top surface of the roughness elements (τ_c) to the total shear stress (τ) is large; in this case, τ_c plays a dominant role and serves as an essential component in the shear-stress partitioning model. Consequently, RM93 is modified by incorporating τ_c into the calculation of τ. Under conditions of λ < 0.32 and H/W > 0.2, the modified RM93 can yield satisfactory predictions regarding the shear-stress partitioning.     

江苏数字地震台网P波谱震级和地震辐射能的计算

基于江苏数字地震台网的宽频带记录,对38次M≥5.0地震的P波谱震级M_P进行测定,对地震的辐射能量进行了估算。结果表明:本文测定的M_P与中国地震台网中心(CENC)测定的MS、德国地学中心(GFZ)测定的MW具有很好的一致性,与该2种震级之间的平均偏差分别约为0.17和0.10级,基本小于世界主要地震机构之间对同一震级的测定误差(约0.2级);同时,基于M_P估算的地震辐射能与基于修正G-R关系由MS震级换算获得的结果十分接近,两者平均能量之比约为1.1,表明M_P与P波群(P+pP+sP)能量流是基本等效的。因此,基于宽频带数字记录测定中强地震的P波谱震级以及地震辐射能是可行的,且测定过程简便。     

某海底沉管隧道风塔及下部结构抗震性能分析

为研究某海底隧道风塔及下部结构体系在塑性阶段的损伤破坏形态及特点,探讨在多重荷载作用下弹塑性静动力响应对结构的影响,建立了沉管隧道风塔及下部结构的大型三维有限元模型。采用基于能量原理的混凝土塑性及损伤本构模型,借助大型有限元软件ANSYS及ABAQUS分别对结构进行不同地震条件下的动力时程分析,对比分析振型、层间位移角及较为完整的塑性损伤破坏系数曲线。结果表明:不同设防地震下,结构整体性良好,振型及层间位移角满足规范要求;不同罕遇地震下,该结构的混凝土塑性拉压损伤最大时刻均发生在20 s,主要破坏区域在风塔与人防井及下部立柱的接触位置,且拉伸破坏系数明显高于压缩破坏。本文的研究成果可以为类似近海沉管隧道工程抗震设计提供一定的依据与指导。     

粘滞阻尼耗能连梁的超高层结构减震性能研究

连梁作为剪力墙结构中的抗震第一道防线,其承载力和耗能能力对整体结构的抗震性能有重要影响。本文提出在连梁中附设粘滞阻尼器,利用阻尼器发生竖向剪切变形而耗能。结合实际工程研究粘滞阻尼耗能连梁的性能,采用ETABS和PERFORM-3D软件对粘滞阻尼耗能连梁结构与传统连梁结构进行有限元模拟对比分析,并对粘滞阻尼耗能连梁的各项最优参数进行研究。结果表明:粘滞阻尼耗能连梁充分发挥耗能作用,整体结构具有良好的抗震性能,与传统连梁结构相比,主体结构的弹性耗能得到明显降低。平面布置方式、竖向布置方式、阻尼器参数的选取对附设粘滞阻尼耗能连梁的框架-核心筒结构减震效果影响较大,合理选择这些参数可以使耗能结构减震效果最优。     

The Venusian induced magnetosphere: A case study of plasma and magnetic field measurements on the Venus Express mission

Plasma and magnetic field measurements made onboard the Venus Express on June 1, 2006, are analyzed and compared with predictions of a global model. It is shown that in the orbit studied, the plasma and magnetic field observations obtained near the North Pole under solar minimum conditions were qualitatively and, in many cases also, quantitatively in agreement with the general picture obtained using a global numerical quasi-neutral hybrid model of the solar wind interaction (HYB-Venus). In instances where the orbit of Venus Express crossed a boundary referred to as the magnetic pileup boundary (MPB), field line tracing supports the suggestion that the MPB separates the region that is magnetically connected to the fluctuating magnetosheath field from a region that is magnetically connected to the induced magnetotail lobes.     

The magnetic field near Mars: A comparison between a hybrid model, Mars Global Surveyor and Mars Express observations

Mars Express (MEX) does not carry its own magnetometer which complicates interpretation of ASPERA-3/MEX ion measurements. The direction of the interplanetary magnetic field (IMF) is especially important because it, among other things, determines the direction of the convective electric field and orientation of the cross tail current sheet and tail lobes. In this paper we present a case study to show the properties of the magnetic field near Mars in a quasi-neutral hybrid (QNH) model at the orbits where the Mars Global Surveyor (MGS) has made measurements, present a method to derive the IMF clock angle by comparing fields in a hybrid model and the direction of the magnetic field measured by MGS by deriving the IMF clock angle. We also use H⁺ ring velocity distribution observations upstream of the bow shock measured by the IMA/ASPERA-3 instrument on board MEX spacecraft. These observations are used to indirectly provide the orientation of the IMF. We use a QNH model (HYB-Mars) where ions are modeled as particles while electrons form a mass-less charge neutralizing fluid. We found that the direct MGS and non-direct IMA observations of the orientation magnetic field vectors in non-crustal magnetic field regions are consistent with the global magnetic field draping pattern predicted by the global model.     

Variations of the magnetic field near Mars caused by magnetic crustal anomalies

The possible avenues for photoelectron transport were determined during southern hemisphere winter at Mars by using a mapping analysis of the theoretical magnetic field. Magnetic field line tracing was performed by superposing two magnetic field models: (1) magnetic field derived from a three-dimensional (3D) self-consistent quasi-neutral hybrid model which does not contain the Martian crustal magnetic anomalies and (2) a 3D map of the magnetic field associated with the magnetic anomalies based on Mars Global Surveyor magnetic field measurements. It was found that magnetic field lines connected to the nightside of the planet are mainly channeled within the optical shadow of the magnetotail whereas magnetic field lines connected to the dayside of the planet are observed to form the remainder of the magnetosphere. The simulation suggests that the crustal anomalies create “a magnetic shield” by decreasing the region near Mars which is magnetically connected to the Martian magnetosphere. The rotation of Mars causes periodic changes in magnetic connectivity, but not to qualitative changes in the overall magnetic field draping around Mars.     

Dependence of the Characteristics of Solar Wind Discontinuities and Shocks with Heliolatitude and Radial Distance

The distribution of the shocks in the heliosphere and their characteristic variations are investigated using Ulysses observations. The jumps in solar wind velocity, IMF magnitude, and proton density across the shocks and discontinuities are evaluated and used to characterize them. The distribution of these discontinuities with respect to heliolatitude ± 80° and with radial distance 1 to 5 AU are analyzed during solar minimum and solar maximum to understand their global behavior. It is noticed that the jumps in solar wind parameters associated with shocks and discontinuities are more prominent during the second orbit of Ulysses, which coincided with the maximum phase of solar activity.