Protection of seismic structures using semi‐active friction TMD

Although the design and applications of linear tuned mass damper (TMD) systems are well developed, nonlinear TMD systems are still in the developing stage. Energy dissipation via friction mechanisms is an effective means for mitigating the vibration of seismic structures. A friction‐type TMD, i.e. a nonlinear TMD, has the advantages of energy dissipation via a friction mechanism without requiring additional damping devices. However, a passive‐friction TMD (PF‐TMD) has such disadvantages as a fixed and pre‐determined slip load and may lose its tuning and energy dissipation abilities when it is in the stick state. A novel semi‐active‐friction TMD (SAF‐TMD) is used to overcome these disadvantages. The proposed SAF‐TMD has the following features. (1) The frictional force of the SAF‐TMD can be regulated in accordance with system responses. (2) The frictional force can be amplified via a braking mechanism. (3) A large TMD stroke can be utilized to enhance control performance. A non‐sticking friction control law, which can keep the SAF‐TMD activated throughout an earthquake with an arbitrary intensity, was applied. The performance of the PF‐TMD and SAF‐TMD systems in protecting seismic structures was investigated numerically. The results demonstrate that the SAF‐TMD performs better than the PF‐TMD and can prevent a residual stroke that may occur in a PF‐TMD system. Copyright © 2009 John Wiley & Sons, Ltd.     

Experiment and analysis of a leverage‐type stiffness‐controllable isolation system for seismic engineering

Owing to the fixed design parameters in traditional isolation systems, the optimal isolation performance may not always be achieved when a structure is subjected to a nondesign earthquake. At the same time, even though an active isolation system (AIS) can offer a better reduction for different seismic waves, in practice the control energy required still constrains its application. To solve this problem, a novel semi‐active isolation system called the Leverage‐type Stiffness Controllable Isolation System (LSCIS) is proposed in this paper. By utilizing a simple leverage mechanism, the isolation stiffness and the isolation period of the LSCIS can be easily controlled by adjusting the position of the pivot point of the leverage arm. The theoretical basis and the control law for the proposed system were first explained in this work, and then a shaking table test was conducted to verify the theory and the feasibility of the LSCIS. As shown in the experiment, the seismic behavior of the LSCIS can be successfully simulated by the theoretical model, and the isolation stiffness can be properly adjusted to reduce the seismic energy input in the LSCIS system. A comparison of the LSCIS with the other systems including passive isolation and AISs has demonstrated that based on the same limitation of base displacement, better acceleration reduction can be achieved by the LSCIS than by any of the other isolation systems. In addition, the control energy required by the LSCIS is lower than that for an AIS using the traditional LQR control algorithm. Copyright © 2010 John Wiley & Sons, Ltd.     

变径洞室超前支护开挖模拟与分析

变径洞室开挖稳定性是地下工程重要的研究课题之一。尤其在围岩软弱的情况下,从小截面向大截面洞室开挖的过程中,会给施工带来很多安全方面的难题。通过有限差分数值分析方法研究了变径洞室的开挖稳定性,分析了拱部小导管超前注浆支护与非超前支护两种施工方法对工程的影响。计算结果表明,由小截面向大截面洞室开挖,不稳定性因素增加,超前小导管注浆支护能够显著提高围岩的稳定性,明显减少了洞室的变形和塑性区,避免了软弱围岩开挖中塌方现象的产生。研究成果对洞室施工具有指导意义。     

顾及形变控制的小屏幕变比例尺交通路线图生成方法

用户在旅游或者室外运动中经常将路线图显示于移动设备上以方便规划路线。然而移动设备显示屏幕通常较小,若较大范围的地图通过等比例尺缩小在小屏幕显示,可能会导致清晰度和辨识度的降低,尤其对于地图中地物较为密集的区域。本文提出一种自动化生成变比例尺地图的方法,通过更加均匀化地图显示内容密度分布以改善地图概览清晰度。在该方法中,首先对密度分布进行估计,密度估计主要考虑地图上路线空间分布以及地标与注记显示空间,然后根据所得到的密度分布进行变比例尺转换,最终生成的变比例尺结果图,其大小取决于给定显示尺寸。相较于现有变比例尺转换方法,本文提出的方法可以考虑了地标与注记显示空间,同时又能有效控制地图变形以提高地图识别。实验结果表明,通过本方法生成变比例尺结果图对地图概览的清晰度有着显著提高,并且能够保持良好的地图识别度。     

基于熵权-IOWGA算子的变权组合预测新方法

针对熵权法组合权重分配固定不变的问题,提出一种基于IOWGA算子的权重分配方法,建立基于熵权-IOWGA算子的变权组合模型。该方法以各单一模型的预测精度作为诱导值,按每一期诱导值的大小对单一模型进行有序赋权,并将其应用到变形数据分析中。实验表明,该方法赋权过程合理,模型预测精度更高,更加适用于变形分析预测过程。     

基桩极限承载力的改进变步长灰色预测模型研究

在深入研究桩土相互作用机理及基桩极限承载力变步长灰色预测方法基础上,针对现有基桩极限承载力灰色预测模型之基桩Q-S曲线导数与背景值确定方法的局限性与不足,结合Q-S曲线发展规律,提出了基桩极限承载能力的改进变步长灰色预测模型与方法,并初步探讨了基桩极限承载力灰色预测方法的精度与可靠性。通过工程实例计算并与同类方法计算结果进行比较分析,表明了所建模型的合理性。     

Theoretical and experimental research on a new system of semi-active structural control with variable stiffness and damping

In this paper, a new system of semi active structural control with active variable stiffness and damping (AVSD) is suggested. This new system amplifies the structural displacement to dissipate more energy, and in turn, effectively reduces the structural response in the case of relatively small story drifts, which occur during earthquakes. A predictive instantaneous optimal control algorithm is established for a SDOF structure equipped with an AVSD system Comparative shaking table tests of a 1/4 scale single story structural model with a full scale control device have been conducted. From the experimental and analytical results, it is shown that when compared to structures without control or with the active variable stiffness control alone, the suggested system exhibits higher efficiency in controlling the structural response, requires less energy input, operates with higher reliability, and can be manufactured at a lower cost and used in a wider range of engineering applications.     

Radial pulsations of helium stars with masses from 1 to 10 <Emphasis Type="Italic">M</Emphasis><Subscript>⊙</Subscript>

We present the results of our hydrodynamic calculations of radial pulsations in helium stars with masses 1 M_⊙ ≤ M ≤ 10 M_⊙, luminosity-to-mass ratios 1 × 10³L_⊙/M_⊙ ≤ L/M ≤ 2 × 10⁴L_⊙/M_⊙, and effective temperatures 2 × 10⁴ K ≤ T_eff ≤ 10⁵ K for mass fractions of helium Y=0.98 and heavy elements Z=0.02. We show that the lower boundary of the pulsation-instability region corresponds to L/M ～ 10³L_⊙/M_⊙ and that the instability region for L/M ? 5 × 10³L_⊙/M_⊙ is bounded by effective temperatures T_eff ? 3 × 10⁴ K. As the luminosity rises, the instability boundary moves into the left part of the Hertzsprung-Russell diagram and radial pulsations can arise in stars with effective temperatures T_eff ? 10⁵ K at L/M ? 7 × 10³L_⊙/M_⊙. The velocity amplitude for the outer boundary of the hydrodynamic model increases with L/M and lies within the range 200 ? ΔU ? 700 km s^?1 for the models under consideration. The periodic shock waves that accompany radial pulsations cause a significant change of the gas-density distribution in the stellar atmosphere, which is described by a dynamic scale height comparable to the stellar radius. The dynamic instability boundary that corresponds to the separation of the outer stellar atmospheric layers at a superparabolic velocity is roughly determined by a luminosity-to-mass ratio L/M ～ 3 × 10⁴L_⊙/M_⊙.     

A spectroscopic study of the secondary star of BM Ori: Preliminary results

Two CCD spectra of the star BM Ori were obtained with the echelle spectrograph of the 6-m telescope. In one of the spectra, a large proportion of lines are distorted by emission. The emission component is blueshifted by 50 km s^?1, suggesting hot-gas outflow from the atmosphere. The equivalent-width ratio of measured lines in the spectra outside and during eclipse is consistent with the assumption that ～2/3 of the primary star’s area is obscured during eclipse, as follows from light curves. Measured line equivalent widths were used to estimate atmospheric parameters of the secondary star, T _eff=7300 K, log g=5.2, and microturbulence ξ_t=6 km s^?1, and to determine its chemical composition. The C, Na, Al, Si, S, Ca, Fe, Ni, and Zn abundances are solar, within the error limits. Li, Sc, Ti, V, Cr, Mn, Co, and Y are overabundant, while Mg, Cu, and Ba are underabundant. In general, the secondary is similar in chemical composition to the star V 1016 Ori. Based on the secondary’s mass determined by solving the radial-velocity curve and on log g estimated spectroscopically from iron ionization equilibrium, we calculated its photospheric radius, R ₂ = 0.5R _⊙. However, the spectroscopic log g=5.2 disagrees with log g=3.5 calculated from the luminosity and effective temperature and with log g=3.0 calculated from light and radial-velocity curves. If the secondary’s photospheric radius is indeed small; this argues for the hypothesis that the eclipsing body is a dust envelope. The radial velocities measured from the two spectra are systematically higher than those calculated from the radial-velocity curve by +34 and +24 km s^?1. It is likely that the secondary’s atmosphere occasionally shrinks.