Stochastic perturbation analysis of groundwater flow. Spatially variable soils,semi-infinite domains and large fluctuations

As is well known, a complete stochastic solution of the stochastic differential equation governing saturated groundwater flow leads to an infinite hierarchy of equations in terms of higher-order moments. Perturbation techniques are commonly used to close this hierarchy, using power-series expansions. These methods are applied by truncating the series after a finite number of terms, and products of random gradients of conductivity and head potential are neglected. Uncertainty regarding the number or terms required to yield a sufficiently accurate result is a significant drawback with the application of power series-based perturbation methods for such problems. Low-order series truncation may be incapable of representing fundamental characteristics of flow and can lead to physically unreasonable and inaccurate solutions of the stochastic flow equation. To support this argument, one-dimensional, steady-state, saturated groundwater flow is examined, for the case of a spatially distributed hydraulic conductivity field. An ordinary power-series perturbation method is used to approximate the mean head, using second-order statistics to characterize the conductivity field. Then an interactive perturbation approach is introduced, which yields improved results compared to low-order, power-series perturbation methods for situations where strong interactions exist between terms in such approximations. The interactive perturbation concept is further developed using Feynman-type diagrams and graph theory, which reduce the original stochastic flow problem to a closed set of equations for the mean and the covariance functions. Both theoretical and practical advantages of diagrammatic solutions are discussed; these include the study of bounded domains and large fluctuations.     

The response of the azimuthal component of the ionospheric electric field to auroral arc brightening

We have analyzed the response of azimuthal component of the ionospheric electric field to auroral arc activity. We have chosen for analysis three intervals of coordinated EISCAT and TV observations on 18 February, 1993. These intervals include three kinds of arc activity: the appearance of a new auroral arc, the gradual brightening of the existing arc and variations of the arc luminosity. The arcs were mostly east-west aligned. In all cases, the enhancement of arc luminosity is accompanied by a decrease in the westward component of the ionospheric electric field. In contrast, an increase of that component seems to be connected with arc fading. The observed response is assumed to have the same nature as the short circuit of an external electric field by the conductor. The possible consequence of this phenomenon is discussed.     

耦合热传导的磁重联的数值模拟

磁重联被认为是太阳耀斑的产生机制,本文数值模拟在日冕中发生在磁重联过程,结果表明耀斑环的表观运动是磁重联的自洽结果;由重联点发出的慢激波对耀斑环的加热有贡献;耀斑环的上升并不意味着重联点的上升。     

顾及地理矢量场空间变化特征的多分辨率纹理可视化方法

网络环境下海量、高维、动态、多尺度地理空间矢量场数据的在线高效可视化,一直是大规模密集矢量场数据集成与综合应用分析亟须解决的关键问题。地理矢量场数据蕴含大量非规则、多尺度、时空异质的变化特征与结构,传统矢量场纹理可视化方法,受全局统一采样密度的限制,存在典型的稠密遮挡、特征模糊的问题。针对上述问题,本文提出了一种顾及地理矢量场空间变化特征的多分辨率纹理可视化方法,引入复合信息熵定量显式描述矢量场的空间变化,以此驱动图像空间内多频噪声纹理生成、矢量场多分辨率纹理的构建与增强表达,有效克服传统纹理可视化方法的技术瓶颈。最后采用风场数据进行试验,验证了本文方法的可靠性与有效性。     

山东省区域地球物理场

山东省各岩石磁性及密度参数基本可分为高、中、低 3类。山东省磁性结晶基底为泰山岩群、荆山群、胶东岩群、胶南岩群。以沂沭断裂带为界 ,山东省区域地球物理场分为鲁东区和鲁西区。鲁东区进一步划分为 3个次级区 ,即北部区、中部区和南部区。鲁西区进一步划分为 5个次级区 ,即鲁北重磁缓变区、鲁西南重高磁高区、中部弧形重磁场区、鲁西中部重低磁高区、鲁中南条带状重磁场区。各区地球物理场由于地质原因各具特点。山东省莫氏面总体呈东浅西深的缓变带 ,在该缓变带的背景上 ,呈周边地区条带状幔隆、中部幔坳的特征。山东省居里面呈近南北向带状分布 ,有德州聊城菏泽隆起带、滨州淄博滕州深坳带、蓬莱海阳千里岩响水隆起带。鲁中隆起北部碰撞带为山东省特殊的构造地带 ,其特征为侵入岩体沿该带断续出现、岩体围岩或岩体内铜及多金属矿化较为普遍、地热田沿该带时有分布、地形上为南部山区和北部平原的分界地带。胶莱盆地内 ,蓼兰—高密缺失莱阳群层位 ;中生代早期 ,盆地东北部与西南部是盆地的沉积中心 ,至晚期盆地中心北移 ,第三纪沉积中心则为平度蓼兰附近 ;盆地较深部位位于诸城凹陷、平度凹陷。胶莱盆地的次级构造单元可划分为 11个 ,七级镇构造带控制了胶莱盆地的成生和发展。山东省岩浆岩通常表     

北淮阳及其邻接区地壳稳定性研究

运用多学科、多技术相结合的研究方法,从现今构造应力场特征、现代地壳形变特征、主干断裂构造以及区域断裂活动性分析、新构造运动、地震活动、数值模拟等方面入手,对北淮阳及其邻接区地壳稳定性进行了全面而系统的研究,指出本区地震活动受走滑活动断裂控制,中、强地震集中于区内东南部和西北部NW向与NE向断裂交汇处;第四纪无大规模差异升降运动;数值模拟等综合分析表明,信阳地区的区域构造稳定性高,现代地壳形变量小,应力平缓,地震活动少且弱。     

The heating of the solar corona

The heating of the solar corona has been a fundamental astrophysical issue for over sixty years. Over the last decade in particular, space-based solar observatories (Yohkoh, SOHO and TRACE) have revealed the complex and often subtle magnetic-field and plasma interactions throughout the solar atmosphere in unprecedented detail. It is now established that any energy release mechanism is magnetic in origin - the challenge posed is to determine what specific heat input is dominating in a given coronal feature throughout the solar cycle. This review outlines a range of possible magnetohydrodynamic (MHD) coronal heating theories, including MHD wave dissipation and MHD reconnection as well as the accumulating observational evidence for quasi-periodic oscillations and small-scale energy bursts occurring in the corona. Also, we describe current attempts to interpret plasma temperature, density and velocity diagnostics in the light of specific localised energy release. The progress in these investigations expected from future solar missions (Solar-B, STEREO, SDO and Solar Orbiter) is also assessed.Received: 6 February 2003, Published online: 14 November 2003 Correspondence to: R. W. Walsh     

Some Comments on the Magnetic Braking of CP Stars

The low rotation velocities of magnetic CP stars are discussed. Arguments against the involvement of the magnetic field in the loss of angular momentum are given: (1) the fields are not strong enough in young stars in the stage of evolution prior to the main sequence; (2) there is no significant statistical correlation between the magnetic field strength and the rotation period of CP stars; (3) stars with short periods have the highest fields; (4) a substantial number of stars with very low magnetic fields (B _e < 500 G) have rotation speeds that are typical of other CP stars; (5) simulations of the magnetic fields by Leroy and the author show that the orientation of dipoles inside rotating stars, both slow and fast, is consistent with an arbitrary orientation of the dipoles; and, (6) slow rotators with P>25 days, which form 12% of the total, probably lie at the edge of the velocity distribution for low mass stars. All of these properties conflict with the hypothesis of magnetic braking of CP stars.     

可用于复杂地质体的波动方程基准面技术

提出改进的波动方程基准面方法,用于解决地表一致性问题,通过基准面的下移,可以使深部的信号增强,变多值走时为单值走时,从根本上消除了上覆层速度横向不均匀的影响,从而可以更好地解决复杂地质体成像问题。作者从原理上对上述观点给予了证明,而且给出利用波动方程基准面有限差分法做的实例－－大庆油田“陆相断隐模型”。