排水粉喷桩加固软土地基桩周土体强度变化规律

排水粉喷桩(2D工法)是同时采用粉喷桩和塑料排水板加固软土地基的一种新工法。在某高速公路中进行了排水粉喷桩加固软土地基的现场试验段施工,分别采用静力触探试验、十字板剪切试验等方法测定加固前及其加固后不同龄期的粉喷桩桩周土强度,得到了施工后桩间土强度变化的规律。测试结果表明采用粉喷桩联合排水板法加固后,桩周土强度有一个先降低后提高的过程,28天龄期时恢复到原状土强度,随着龄期的增长桩周土强度可以进一步增加。最后对桩周土强度的变化机理进行了初步探讨。     

边（滑）坡治理中h型组合抗滑桩的分析方法及工程应用

h型组合抗滑桩是用横梁连接前后两排桩外形似h型的可抵抗大滑坡推力的支挡结构,分析了h型桩支挡边（滑）坡的作用机理,根据其受力特征,可以滑面为界将其分为上下两个部分计算分析,通过室内试验研究和理论分析,提出可按在滑坡推力作用下的横向弹性地基约束的平面刚架模型分析上半部分（受荷段）结构内力,其间考虑了桩排间的坡体压力作用,在此基础上可对下半部分（锚固段）直接按弹性地基梁理论计算,按所提出的方法设计计算的h型桩成功用于四川广巴高速公路一大型堆积体路堑边坡工程中,取得了良好的实际效果。     

桩锚挡墙联合支护残积土边坡离心模型试验研究

利用土工离心机分别对钢轨桩、锚杆联合重力式挡土墙支护土质边坡的效果进行模型对比试验研究,分析了钢轨桩和锚杆在重力式挡土墙支护土质边坡中的作用。试验结果表明,强降雨诱发重力式挡土墙支护下的残积土边坡产生滑动变形,对边坡稳定构成威胁;挡土墙下打入钢轨桩联合支护土质边坡会大大降低因降雨产生的墙体偏移,但墙顶上部坡体的局部浅层滑动仍不可避免;植入墙顶上部坡体内并锚固于墙身的锚杆对边坡局部浅层滑动起到了很好的抑制作用。在不增加挡墙自重前提下,钢轨桩下延作用以及锚杆锚固作用提升了挡土墙的抗倾覆能力和边坡浅层抗滑塌能力,从坡体内部和浅层同时改善了重力式挡土墙的支护效果;钢轨桩和锚杆的使用均布了挡土墙背部土压力,有效避免了局部应力集中。     

卫星重力梯度数据粗差探测方法的比较研究

比较研究了卫星重力梯度数据粗差探测的阈值法、Grubbs检验、Dixon检验和小波分析法及组合方法。基于卫星重力梯度测量粗差的来源和特征,模拟生成了重力梯度数据的粗差,利用上述粗差探测方法模拟计算的结果表明：联合Dixon检验和小波分析的组合法最有效。     

合肥地区深基坑支护设计与施工初探

深基坑工程的支护结构形式决定了基坑工程的安全性和经济性。文章介绍了深基坑在复杂条件下分别采用土钉墙支护与桩锚联合支护的不同效果。对类似深基坑开挖支护设计与施工具有一定的借鉴作用。并对施工中存在的问题进行了分析探讨。     

中国大陆地壳运动的GPS观测及相关动力学研究

现代空载大地测量技术的发展极大地改变了传统大地测量学的观测手段、研究内容和范围,促进了地球动力学领域的研究．本文回顾过去近二十年来在中国大陆进行的全国及区域性GPS观测和取得的成果,重点评述在GPS相关动力学领域的研究进展和存在的问题,对我国GPS观测及动力学研究今后的发展提出初步见解．     

Cassini UVIS observations of the Io plasma torus: IV. Modeling temporal and azimuthal variability

In this fourth paper in a series, we present a model of the remarkable temporal and azimuthal variability of the Io plasma torus observed during the Cassini encounter with Jupiter. Over a period of three months, the Cassini Ultraviolet Imaging Spectrograph (UVIS) observed a dramatic variation in the average torus composition. Superimposed on this long-term variation, is a 10.07-h periodicity caused by an azimuthal variation in plasma composition subcorotating relative to System III longitude. Quite surprisingly, the amplitude of the azimuthal variation appears to be modulated at the beat frequency between the System III period and the observed 10.07-h period. Previously, we have successfully modeled the months-long compositional change by supposing a factor of three increase in the amount of material supplied to Io's extended neutral clouds. Here, we extend our torus chemistry model to include an azimuthal dimension. We postulate the existence of two azimuthal variations in the number of superthermal electrons in the torus: a primary variation that subcorotates with a period of 10.07 h and a secondary variation that remains fixed in System III longitude. Using these two hot electron variations, our model can reproduce the observed temporal and azimuthal variations observed by Cassini UVIS.     

First definitive observations of meteor shower particles using a high-power large-aperture radar

We present the first clear observations of meteor shower activity from meteor-head echoes detected by a high-power large-aperture radar (HPLAR). Such observations have been performed at the Jicamarca VHF radar using its interferometric capabilities allowing the discrimination of meteor shower echoes from the much more frequent sporadic meteors. Until now, HPLARs were unable to distinguish meteor shower from the much more common sporadic meteor ones. In this work we have been able to detect and characterize the η-Aquariids (ETA) as well as the Perseids (PER) showers. The shower activity is more conspicuous for the ETA than for the PER shower due to the more favorable geometry. Namely, PER meteors come from low elevation angles, experiencing more filtering due to the combined Earth-atmosphere-radar instrument. In both cases, there is an excellent agreement between the measured mean velocity of the shower echoes and their expected velocity, within a fraction of 1 km s⁻¹. Besides the good agreement with expected visual results, HPLARs observe meteors with a variety of particles sizes and masses, not observed by any other technique. Taking into account the different viewing volumes, compare to optical observations Jicamarca observes more than 1000 times more ETA meteors. Our results indicate that Jicamarca and other HPLARs are able to detect the echoes from meteor showers, but without interferometric capabilities such populations are difficult to identify just from their velocity distributions, particularly if their velocity distributions are expected to be similar to the more dominant distributions of sporadic meteors.     

Observations of atmospheric water vapor above the Tharsis volcanoes on Mars with the OMEGA/MEx imaging spectrometer

The OMEGA imaging spectrometer onboard the Mars Express spacecraft is particularly well suited to study in detail specific regions of Mars, thanks to its high spatial resolution and its high signal-to-noise ratio. We investigate the behavior of atmospheric water vapor over the four big volcanoes located on the Tharsis plateau (Olympus, Ascraeus, Pavonis and Arsia Mons) using the 2.6 μm band, which is the strongest and most sensitive H₂O band in the OMEGA spectral range. Our data sample covers the end of MY26 and the whole MY27, with gaps only in the late northern spring and in northern autumn. The most striking result of our retrievals is the increase of water vapor mixing ratio from the valley to the summit of volcanoes. Corresponding column density is often almost constant, despite a factor of ∼5 decrease in air mass from the bottom to the top. This peculiar water enrichment on the volcanoes is present in 75% of the orbits in our sample. The seasonal distribution of such enrichment hints at a seasonal dependence, with a minimum during the northern summer and a maximum around the northern spring equinox. The enrichment possibly also has a diurnal trend, being the orbits with a high degree of enrichment concentrated in the early morning. However, the season and the solar time of the observations, due to the motion of the spacecraft, are correlated, then the two dependences cannot be clearly disentangled. Several orbits exhibit also spatially localized enrichment structures, usually ring- or crescent-shaped. We retrieve also the height of the saturation level over the volcanoes. The results show a strong minimum around the aphelion season, due to the low temperatures, while it raises quickly before and after this period. The enrichment is possibly generated by the local circulation characteristic of the volcano region, which can transport upslope significant quantities of water vapor. The low altitude of the saturation level during the early summer can then hinder the transport of water during this season. The influence of the coupling between atmosphere and surface, due mainly to the action of the regoliths, can also contribute partially to the observed phenomenon.