Robust and reliable metamodels for mechanized tunnel simulations

The main objective of this paper is to construct a robust and reliable metamodel for the mechanized tunnel simulation in computationally expensive applications. To accomplish this, four metamodeling approaches have been implemented and their performance has been systematically evaluated through a comparative study utilizing pure mathematical test functions. These metamodels are quadratic polynomial regression, moving least squares, proper orthogonal decomposition with radial basis functions, and an extended version of the latest approach. This extended version has been proposed by the authors and named proper orthogonal decomposition with extended radial basis functions. After that, a system identification study for mechanized tunneling has been conducted through the back analysis of synthetic measurements. In this study, the best performing metamodel, that is the one suggested by the authors, has been employed to surrogate a complex and computationally expensive 3D finite element simulation of the mechanized tunnel. The obtained results demonstrate that the proposed metamodel can reliably replace the finite element simulation model and drastically reduce the expensive computation time of the back analysis subroutine.     

全球超大城市空间扩张及分形特征研究

超大城市是全球经济、文化以及高科技产业发展的承载体和重要纽带,其形态结构特征和人口聚集效应是城市化影响的典型表现,然而当前对于全球超大城市形态特征及扩张模式的研究相对不足。基于2000—2020年全球城市土地利用/覆盖变化数据（GULUC-30）,利用城市扩张强度差异指数分析了超大城市用地的时空变化规律;而后运用面积—半径标度分析模型研究了超大城市的分形特征及扩张模式,最后基于城市用地面积和城市人口之间的线性关系评价城市用地效率。结果发现：① 2000—2020年东南亚和东亚的中国超大城市用地扩张最剧烈,城市用地面积分别扩张了3148.32 km²和5996.26 km²,城市扩张强度差异指数平均值大于3;② 2000—2020年超大城市的形态特征和扩张模式向着更加集约和紧凑的方向发展,径向维数平均值由1.54增加至1.56,分维差呈逐年减少趋势,城市内部结构一体化特征显著;③ 北美和欧洲的超大城市用地效率低,2020年城市用地面积与城市人口比值系数范围为0.89~4.11;南亚和非洲城市用地效率高,比值范围为0.23~0.87。超大城市空间扩张格局和形态变化的认识对于城市用地的集约利用和可持续发展具有重要参考价值。严格控制超大城市扩张规模,促进城市用地的均衡发展是建设韧性城市和实现城市地区可持续发展的必要条件。     

Spectroscopic binaries near the north Galactic Pole

Orbits based principally on radial-velocity measurements made with the Haute-Provence Coravel spectrometer are presented for eight binary systems which include some of the faintest HD stars in the Galactic-Pole field. They are HD 103418 (which is double-lined), 105021, 108151, 113169, 113323, 113650, 113714, and 116514. Their periods range from 3.7 to 15.1 days. Very little else is known about any of them.     

Spectroscopy and orbit determination of the chromospherically active double-lined binary system HD 163621 = V835 Herculis

HD 163621 is a double-lined spectroscopic binary in a circular orbit whose period is 3.3 days. Spectral classification of the components has proved difficult, but current results of K0 V and late K V are reasonably consistent with our best model of the system, which has spectral types of G8V and K7V. The object shows photometric variability and chromospheric activity and is therefore a member of the BY Draconis class of variables. The minimum masses are quite small, 0.10 and 0.07 M⊙ for the primary and secondary, respectively, suggesting an orbital inclination of about 30°. The system is synchronously rotating. Its distance is estimated to be 31 pc, which makes it an excellent candidate for a trigonometric parallax determination. Kitt Peak National Observatory, [U.S.] National Optical Astronomy Observatories, operated by AURA Inc. under contract with the [U.S.] National Science Foundation.     

煤矿井下定向钻孔中电阻率探测技术与应用

受高瓦斯/承压奥灰水威胁的工作面开采前,一般采取定向钻进技术在工作面底板开展压裂或注浆工程保障开采安全。利用底板定向钻孔开展孔中探测工作,可更加精细揭露工作面内隐伏构造,还可实现“一孔多用”。为解决定向钻孔内的探测问题,提出一种在水平定向钻孔中进行直流电阻率法探查的方法。定向钻孔施工完毕后,退出定向钻孔施工的通缆钻杆,送入内平钻杆,将孔中高密度电缆通过钻杆尾端特制水便送入钻孔,使孔中电缆平铺于钻孔中,在定向钻孔水平段,进行孔内直流电阻率法径向探测。在理论上通过数值模拟研究层状介质下单孔测量工作模式的接收信号衰减规律、视电阻率曲线变化特征、顶底板岩性对测量结果的影响等,并采用单孔测量数据对孔旁异常范围进行反演定位。数值模拟研究表明,孔中电阻率探测方法对隐伏的异常体有良好的探测效果。通过在陕西韩城某矿井下实际煤层底板探测试验,对研究区2个定向抽采钻孔孔中探测数据进行处理,反演结果异常区与工作面内隐伏小断层位置吻合,验证了定向钻孔中电缆布置的可行性和定向钻孔内通过孔内径向和孔间透视探测隐伏构造的可靠性。      

基于3D-DIC的砂岩裂纹扩展及损伤监测试验研究

裂纹监测对岩石损伤演化的认识至关重要。为研究岩石裂纹扩展及损伤变形特性,开展了含不同倾角（0°～90°）预制裂隙的标准细黄砂岩样的单轴压缩试验。利用三维数字图像相关技术（3D-DIC）获取岩样三维空间坐标下的应变分布,并结合声发射从光学与声学的角度监测了裂纹的扩展演化。由此提出了一种裂纹主应变的计算方法,定量表征岩石劣化的损伤变量D值。最后,探讨了由声发射与损伤变量D值确定岩样特征强度的影响因素。结论如下：（1）裂纹主应变反映了岩样受荷过程中同源裂纹在时间上的变化速率与空间上的扩展趋势,能较好地表征岩石的开裂行为;（2）声发射适用于确定岩样的起裂应力,不适用于损伤应力的确定,损伤变量D值所确定的起裂应力滞后于声发射,但适用于损伤应力特征值的确定;（3）结合声发射与DIC技术确定的归一化起裂应力范围为0.63～0.94、归一化损伤应力的范围为0.83～0.99;（4）预有裂隙会影响岩石的材料力学性能。随着倾角的增加,岩石的起裂应力、损伤应力及峰值应力呈增长的趋势,由于难以形成局部应变场聚集,裂纹的萌生与起裂更加困难。结果表明,3D-DIC技术的利用可以提高对岩石开裂行为的理解,对岩石的损伤监测与判识更有重要的意义。     

裂隙黄土边坡三维稳定性极限分析

黄土边坡中竖直裂隙的发育往往会对边坡稳定产生影响。相对于平面应变机制,建立三维破坏机制下边坡稳定性分析方法更能接近实际边坡失稳情况。基于塑性极限分析上限法,考虑预先存在竖直裂隙的三维黄土边坡不同破坏机制（坡面破坏、坡脚破坏和坡底破坏）,建立能量平衡方程及其无量纲临界高度值γH/c表达式,采用随机搜索法得到了临界高度的上限解。分析了约束宽度、边坡坡度、内摩擦角以及裂隙深度对三维竖直裂隙黄土边坡临界高度值的影响。结果表明：对于坡脚破坏机制,临界高度值随着裂隙深度的增加而减小,减小至临界裂隙深度 (δ /H)_min后,裂隙深度的增加不再影响临界高度值;临界裂隙深度随着坡度β 的增大而增大,随着内摩擦角φ 的增大而减小。当约束宽度B/H<0.8时,大多数破坏机制为坡面破坏。当约束宽度B/H=0.8、内摩擦角φ =10° 及约束宽度B/H=0.6、内摩擦角φ =15° 时,边坡的破坏从坡面破坏机制逐渐过渡到坡脚破坏机制。存在竖直裂隙的黄土边坡比完整边坡具有更小的临界高度,约束宽度及内摩擦角会对三维黄土边坡破坏机制产生影响。     

比例射线移位算法的改进及其应用

点状要素群移位的比例射线算法能够较好地保持移位后点群的空间分布模式。文中从农村居民地群移位的实际要求出发,对比例射线移位算法进行了改进:首先考虑居民地面积的不同大小对移位的影响;其次,设计比例射线移位的迭代方法;最后对于非常邻近的居民地群的移位,采用"微小"移位方法。通过实验验所改进的算法是有效的。     

Time‐series high‐resolution spectroscopy and photometry of ε Aurigae from 2006–2013: Another brick in the wall

We present continuous and time‐resolved R = 55 000 optical échelle spectroscopy of ε Aurigae from 2006–2013. Data were taken with the STELLA Echelle Spectrograph of the robotic STELLA facility at the Observatorio del Teide in Tenerife. Contemporaneous photometry with the Automatic Photoelectric Telescopes at Fairborn Observatory in Arizona is presented for the years 1996–2013. Spectroscopic observations started three years prior to the photometric eclipse and are still ongoing. A total of 474 high‐resolution échelle spectra are analyzed and made available in this paper. We identify 368 absorption lines of which 161 lines show the characteristic sharp disk lines during eclipse. Another 207 spectral lines appeared nearly unaffected by the eclipse. From spectrum synthesis, we obtained the supergiant atmospheric parameters T_eff = 7395 ± 70 K, log g ≈ 1, and [Fe/H] = +0.02 ± 0.2 with ξ_t = 9 km s^–1, ζ_RT = 13 km s^–1, and v sin i = 28 ± 3 km s^–1. The residual average line broadening expressed in km s^–1 varies with a period of 62.6 ± 0.7 d, in particular at egress and after the eclipse. Two‐dimensional line‐profile periodograms show several periods, the strongest with ≈110 d evident in optically thin lines as well as in the Balmer lines. Center‐of‐intensity weighted radial velocities of individual spectral lines also show the 110‐d period but, again, additional shorter and longer periods are evident and are different in the Balmer lines. The two main spectroscopic Hα periods, ≈ 116 d from the line core and ≈ 150 d from the center‐of‐intensity radial velocities, appear at 102 d and 139 d in the photometry. The Hβ and Johnson V I photometry on the other hand shows two well‐defined and phase‐coherent periods of 77 d and 132 d. We conclude that Hα is contaminated by changes in the circumstellar environment while the Hβ and V I photometry stems predominantly from the non radial pulsations of the F0 supergiant. We isolate the disk‐rotation profile from 61 absorption lines and found that low disk eccentricity generally relates to low disk rotational velocity (but not always) while high disk eccentricity always relates to high velocity. There is also the general trend that the disk‐absorption in spectral lines with higher excitation potential comes from disk regions with higher eccentricity and thus also with higher rotational velocity. The dependency on transition probability is more complex and shows a bi‐modal trend. The outskirts of the disk is distributed asymmetrically around the disk and appears to have been built up mostly in a tail along the orbit behind the secondary. Our data show that this tail continues to eclipse the F0 Iab primary star even two years after the end of the photometric eclipse. High‐resolution spectra were also taken of the other, bona‐fide, visual‐binary components of ε Aur (ADS 3605BCDE). Only the C‐component, a K3‐4‐giant, appears at the same distance than ε Aur but its radial velocity is in disagreement with a bound orbit. The other components are a nearby (≈ 7 pc) cool DA white dwarf, a G8 dwarf, and a B9 supergiant, and not related to ε Aur. The cool white dwarf shows strong DIB lines that suggest the existence of a debris disk around this star. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)