Preliminary design recommendations for dip-slip fault–foundation interaction

The article outlines the main findings and conclusions of the QUAKER research project and other related studies on the behaviour of foundations built on top of a rupturing dip-slip fault. Although emphasis is placed on normal faults, the derived conclusions are valid for reverse faults, as well. A key conclusion is that it is quite feasible to design a foundation to withstand an underneath rupturing fault. Practical design recommendations suitable for developing future Code requirements on the subject, are developed on the basis of the presented conclusions.     

从中国、美国、欧洲抗震设计规范谱的比较 探讨我国的抗震设计反应谱

本文分析了中国、美国、欧洲 3 种抗震设计规范的地震动参数取值,并比较了 3 种抗震设计反应谱。结果表明,总体上说,欧洲、美国规范的加速度短周期反应谱高于中国规范。但随着周期的扩大,由于中国规范中反应谱的下降指数较小,导致了中国规范中的反应谱逐渐接近并可能超过了欧洲、美国规范。本文的结果可为我国未来抗震设计规范修订,以及地震安全性评价工作中确定设计反应谱提供参考。     

Transition of solar cycle length in association with the occurrence of grand solar minima indicated by radiocarbon content in tree-rings

In this paper, we review the variation of the 11-year solar cycle since the 15th century revealed by the measurement of radiocarbon content in single-year tree-rings of Japanese cedar trees. Measurements of radiocarbon content in absolutely dated tree-rings provide a calibration curve for accurate dating of archaeological matters, but at the same time, enable us to examine the variations of solar magnetic activity in the pre-historical period. The Sun holds several long-term quasi-cyclic variations in addition to the fundamental 11-year sunspot activity cycle and the 22-year polarity reversal cycle, and it is speculated that the property of the 11-year and the 22-year solar cycle varies in association with such long-term quasi-cycles. It is essential to reveal the details of solar variations around the transition time of solar dynamo for illuminating the mechanisms of the long-term solar variations. We therefore have investigated the property of the 11-year and 22-year cycles around the two grand solar minima; the Maunder Minimum (1645–1715 AD) and the Spoerer Minimum (1415–1534 AD), the periods of prolonged sunspot minima. As a result, slight stretching of the “11-year” and the “22-year” solar cycles was found during these two grand solar activity minima; continuously during the Maunder Minimum and only intermittently during the Spoerer Minimum. On the contrary, normal or slightly shortened 11-year cycles were detected during the interval period of these two minima. It suggests the inverse correlation between the solar cycle length and solar magnetic activity level, and also the change of meridional flow during the grand solar activity minima. Further measurements for the beginning of the grand solar minima will provide a clue to the occurrence of such prolonged sunspot disappearance. We also discuss the effect of solar variations to radiocarbon dating.     

Preliminary results on the fundamental parameters of the eclipsing binary V398 Lacertae

The Hipparcos Space Astrometry Mission photometric observations of V398 Lac, led to the discovery of its variability, allowing to classify it as an eclipsing binary with an orbital period of about 5.4 days. This prompted us to acquire highresolution échelle spectra with the aim of performing accurate radial velocity measurements and to determine the main physical parameters of the system's components. We present, for the first time, a double‐lined radial velocity curve and determine the orbital and physical parameters of the two components, that can be classified both as late B‐type stars. In particular, we obtained an orbital inclination i ∼ 85°. With this value of the inclination, we deduced masses M₁ = 3.83±0.35 M_⊙ andM₂ = 3.29±0.32 M_⊙, and radii R₁ = 4.89±0.18 R_⊙ and R₂ = 2.45±0.11 R_⊙ for the more massive and less massive components, respectively. Both components are well inside their own Roche lobes. The mass ratio is M₂/M₁ ∼ 0.86. We derived also the projected rotational velocities as v₁ sin i = 79±2 km s^–1 and v² sin i = 19±2 km s^–1. Our measurements indicate that the rotation of the primary star is essentially pseudo‐synchronized with the orbital velocity at the periastron, while the secondary appears to rotate very slowly and has not yet attained synchronization. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

地形三维可视化处理中几个问题的探讨

以长江中上游地区作为试验区,针对利用ERDAS IMAGINE V8．7制作三维飞行漫游时中文注记的生成、不同空间分辨率DEM的地形信息载量与内存消耗的关系、EDM与卫星影像叠加后在不同地形环境下的参数设置、三维飞行漫游文件格式等问题,提出了一系列切实可行的解决方案,在实践中取得了较好的三维可视化效果。研究结果对于城市景观规划设计、土地资源环境调查等诸多领域,都具有很强的实用价值。     

春季一次典型强对流单体降雹雷达产品特征分析

利用文山新一代天气雷达回波资料及PUP提供的雷达产品对2008年4月12日下午发生在文山州东北部的强对流降雹过程进行分析。结果表明：此次强对流风暴表现为一带状单体强降雹回波分裂为2条EN-W S向带状强对流回波带。在两条带状回波沿雷达径向的伸展方向又有多个强对流回波单体的生成发展。在强对流发展旺盛阶段一直有风向辐合和逆风区伴随。最大回波强度达61.2 dB z,≥50 dB z的强回波高度,最高≥10 km,回波垂直伸展高度大于13 km,最高≥16 km。在强对流风暴发展旺盛阶段,相应的垂直液态水含量和密度分别超过50kg/m2和10 kg/m2,最大达55 kg/m2。强降雹过程具有非常典型的冰雹云回波特征：＂V＂型缺口、回波悬垂结构、回波墙及有界弱回波区非常明显。     

High-resolution spectroscopy of V854 Cen in decline – absorption and emission lines of C2 molecules

High-resolution optical spectra of the R Coronae Borealis (RCB) star V854 Centauri in the early stages of a decline show, in addition to the features reported for other RCBs in decline, narrow absorption lines from the C₂ Phillips system. The low rotational temperature, T _rot=1150 K, of the C₂ ground electronic state suggests the cold gas is associated with the developing shroud of carbon dust. These absorption lines were not seen at a fainter magnitude on the rise from minimum light, nor at maximum light. This is the first detection of cold gas around an RCB star.     

The evolution of a rapidly accreting helium white dwarf to become a low-luminosity helium star

We have examined the evolution of merged low-mass double white dwarfs which become low-luminosity (or high-gravity) extreme helium stars. We have approximated the merging process by the rapid accretion of matter, consisting mostly of helium, on to a helium white dwarf. After a certain mass is accumulated, a helium shell flash occurs, the radius and luminosity increase and the star becomes a yellow giant. Mass accretion is stopped artificially when the total mass reaches a pre-determined value. As the helium-burning shell moves inwards with repeating shell flashes, the effective temperature gradually increases as the star evolves towards the helium main sequence. When the mass interior to the helium‐burning shell is approximately 0.25 M_⊙, the star enters a regime where it is pulsationally unstable. We have obtained radial pulsation periods for these models.
These models have properties very similar to those of the pulsating helium star V652 Her. We have compared the rate of period change of the theoretical models with that observed in V652 Her, as well as with its position on the Hertzsprung–Russell diagram. We conclude that the merger between two helium white dwarfs can produce a star with properties remarkably similar to those observed in at least one extreme helium star, and is a viable model for their evolutionary origin. Such helium stars will evolve to become hot subdwarfs close to the helium main sequence. We also discuss the number of low-luminosity helium stars in the Galaxy expected for our evolution scenario.     

Colliding winds in V1016 Cygni

We present MERLIN observations of the symbiotic nova V1016 Cygni made at 6 cm between 1992 and 1997 and at 18 cm in 1993 and 1997. In the 6-cm images we find complex structure which has not been previously seen, in particular three bright components. These components do not appear to be expanding as would be expected from the remains of a hot wind resulting from the nova outburst. The change in positions of two of the features exhibits tentative east–west movement. The brightness temperature of the peak with the highest flux density remains above 50 000 K in all epochs, thereby confirming the presence of shocked material in the system. At 18 cm there is no evidence of any non-thermal emission as might be expected from comparison with a sister star, HM Sge.