Optimized running conditions and sensitivity for direction sensitive detectors of WIMP dark matter

Optimum fill pressures for direction-sensitive dark matter detectors based on tracking in gases are considered. Given the minimum resolvable track length and the gas fill, the Lindhard–Scharf stopping model leads to the existence of an optimum pressure which maximizes the specific event rate R (event rate per unit detector volume). In addition, maximizing the detectibility of the recoil nucleus diurnal asymmetry is considered. Optimum fill pressures are calculated for Ar, CF₄, CS₂ and Xe gas fills, as a function of the WIMP mass and the minimum resolvable track length. The associated minimum target volumes required to achieve currently competitive WIMP-nucleon cross-section sensitivity are also calculated. The standard isothermal sphere model of the galactic WIMP halo is used throughout, but the method could be extended to use any desired WIMP distribution function.     

Development dynamics of intense solar proton flares

We consider the relationship of electromagnetic radiation in the three most intense flares of solar cycle 23, more specifically, those of October 28, 2003, January 20, 2005, and September 7, 2005, to the acceleration and release of protons into interplanetary space. The impulsive phase of these flares lasted ～ 20 min and consisted of at least three energy release episodes, which differed by their manifestation in the soft (1–8 Å, GOES) and hard (>150 keV, INTEGRAL) X-ray ranges as well as at radio frequencies of 245 MHz and 8.8 GHz. The protons and electrons were accelerated in each episode, but with a different efficiency; the relativistic protons were accelerated only after 5–6min of impulsive-phase development after the onset of a coronal mass ejection. It is at this time that maximum hard X-ray fluxes were observed in the September 7, 2005 event, which exceeded severalfold those for the other two flares considered. We associate the record fluxes of protons with energies > 200MeV observed in the heliosphere in the September 7, 2005 event with the dynamics of the impulsive phase. The extreme intensities of the microwave emission in the October 28, 2003 and January 20, 2005 events were probably attributable to the high-energy electron trapping conditions and did not reflect the acceleration process.     

On the acceleration of solar-flare charged particles in a collapsing magnetic trap with an electric potential

We consider the kinetic problem of charged-particle acceleration in a magnetic trap with converging magnetic mirrors. We show that for a positive electrostatic potential of the trap plasma relative to the mirrors, the efficiency of confinement and acceleration increases for electrons and decreases for ions.     

Evolution of the photospheric magnetic field and coronal null points before solar flares

Based on a topological model for the magnetic field of a solar active region (AR), we suggest a criterion for the existence of magnetic null points on the separators in the corona. With the problem of predicting solar flares in mind, we have revealed a model parameter whose decrease means that the AR evolves toward a major eruptive flare. We analyze the magnetic field evolution for AR 9077 within two days before the Bastille Day flare on July 14, 2000. The coronal conditions are shown to have become more favorable for magnetic reconnection, which led to a 3B/X5.7 eruptive flare.     

Behavior of Weak Soils Reinforced with End-Bearing Soil-Cement Columns Formed by the Deep Mixing Method

This article reports on a series of small-scale, plane strain, 1 g physical model tests designed to investigate the bearing capacity and failure mechanics of end-bearing soil-cement columns formed via Deep Mixing (DM). Pre-formed soil-cement columns, 24 mm in diameter and 200 mm in length, were installed in a soft clay bed using a replacement method; the columns represented improvement area ratios, a_p, of 17%, 26%, and 35% beneath a rigid foundation of width 100 mm. Particle Image Velocimetry (PIV) was implemented in conjunction with close-range photogrammetry in order to track soil displacement during loading, from which the failure mechanisms were derived. Bearing capacity performance was verified using Ultimate Limit State numerical analysis, with the results comparing favorably to the analytical static and kinematic solutions proposed by previous researchers. A new equation for bearing capacity was derived from this numerical analysis based on the improvement area ratio and cohesion ratio of the soil column and ground model.     

细粒含量对冰碛土抗剪强度影响的实验研究

为研究细粒组颗粒在浸水/降雨条件下产生迁移对冰碛土抗剪强度的影响,从西藏林芝市帕隆藏布嘎隆寺沟流域内采取冰碛土样品,进行7种不同细粒（粒径小于2 mm）含量情况下的冰碛土比重和相对密度的测试,开展了不同围压下的大型饱和固结不排水三轴（CU）实验。结果表明：（1）细粒含量对干密度的影响较小,不同细粒含量的冰碛土孔隙比大致相同,细颗粒对孔隙具有改造作用,不同细粒含量会引起孔隙结构的差异,从而导致冰碛土的结构差异,最终导致抗剪强度的不同;（2）细颗粒迁移导致冰碛堤坡脚和内部一定深度细粒含量较高,达到一定的量值时,抗剪强度明显降低,冰碛堤容易发生剪切破坏;（3）细粒含量对抗剪强度参数的变化具有重要影响,从中还可以反映出冰碛土结构控制的变化：粗颗粒控制→粗细颗粒共同控制→细颗粒控制。研究结果对于评价冰碛堤的稳定性具有重要意义。     

A comprehensive study on the parameters setting in smoothed particle hydrodynamics (SPH) method applied to hydrodynamics problems

Smoothed particle hydrodynamics (SPH) is a meshfree, Lagrangian particle method which has advantages in handling solids with extremely large deformation. Like any other numerical methods, cares must be taken to ensure its desirable accuracy and stability through considering several correction techniques in calculation. The selection of values for parameters in those correction approaches is a key step in SPH simulation, which is always difficult for new beginners to deal well with effectively. This paper examines the common inconsistency and instability problems in SPH method and studies its computational efficiency when applied to hydrodynamics problems with material strength like soil column collapse. We analyzed in detail how the correction techniques mitigate these inconsistency and instability problems. Also, the numerical testing results associate with different values for the parameters used in the correction techniques are provided for better understanding the influence of these parameters and for finding out the desirable values. It is found that (1) the SPH method is easily subjected to an inconsistency problem in the boundary area due to the boundary deficiency, and it can be treated well by adopting “virtual particles” contributing to the particle summations. (2) The numerical oscillation in SPH simulation can be mitigated effectively by artificial viscosity with the suggested parameter values. (3) The tension cracking treatment, artificial viscosity and artificial stress work well in removing the tensile instability problem in SPH method. In addition, the nearest neighboring particle searching (NNPS) algorithm, spacing ratio, smoothing length and time step influence the efficiency and accuracy of SPH method significantly. It is shown that SPH method with suggested parameters values can produce a very good result compared with the experimental result.     

基于测试粒子模拟的垂直无碰撞激波对离子的加速研究

本文利用测试粒子模拟的方法研究离子在通过垂直无碰撞激波结构时的加速.我们首先探究了在理想激波条件下,离子通过激波结构后的能量增益与其初始参数(包括回旋相位角、初始位置和上游平均能量)的关系; 然后进一步探索了离子通过由自洽的一维混合模拟给出的更接近真实的激波结构时获得的加速,研究了激波内部的电场和磁场结构对离子能量增益的影响.结果显示,当离子能量较低(离子回旋半径小于激波面厚度或相当)时,激波横越电势和磁过冲对离子的能量增益起到促进作用; 而当能量较高时,激波内部结构对于离子能量增益的影响逐渐可以忽略. 此外,与激波横越电势相比,激波磁过冲的强度对离子能量增益的影响占主导,离子的能量增益随着磁过冲的增强而增强.最后,我们发现激波的磁场过冲和横越电势对于离子能量增益的影响之间的关系比较复杂,不能简单叠加,甚至有互相抵消的效应.作为示例,我们给出了一个激波法向电场的双极结构使得离子加速变弱的例证.

     

海洋浮游微食物网生物在海洋颗粒形成和沉降中的作用

海洋中存在着大量的颗粒,包括大型聚合颗粒（即海雪,粒径>500μm）、小型聚合颗粒（1~500μm）和亚微米颗粒粒径（<1μm）等。颗粒在海水中营造了不同于纯海水的小生境,其中生活着与自然海水中不同的生物。异养细菌、蓝细菌、真核藻类、鞭毛虫、纤毛虫等微食物网生物可以黏附在海洋颗粒上,或生活在颗粒内部,其丰度高于周围水体中的自由生活生物,这可能是由于颗粒提供了更适宜生长的营养环境。本文综述了海洋浮游微食物网生物在海洋颗粒形成和沉降中的作用。微食物网生物在颗粒物的形成过程中起到很重要的作用,它们可以直接促进颗粒形成,也可以彼此结合成颗粒,或微型浮游动物排粪形成颗粒。微食物网生物还可以对颗粒进行转化,影响颗粒的大小、沉降速度、或对颗粒及其黏附生物进行摄食。微食物网生物由于本身较小,沉降较慢,但这些生物和颗粒的结合使得微食物网生物在碳通量中发挥重要的作用。     

苏里格气田北部下石盒子组盒8段沉积微相研究

通过对苏里格气田北部20余口钻井岩心的岩石学特征、沉积构造、剖面结构的详细研究,结合测井相标志和古生物标志,认为苏里格气田北部盒8段属辫状河沉积,发育河道和洪泛平原两个亚相。河道亚相可进一步划分为河床底部滞留沉积和心滩两个微相,往往组成向上变细的剖面结构,测井曲线一般为中-高幅的齿化或微齿化的箱形或钟形;洪泛平原亚相在剖面结构上表现为砂泥岩的不等厚互层,测井曲线多呈锯齿状。在微相分析的基础上,编制了盒8上和盒8下两个时期的沉积微相平面图,其显示出河道心滩砂体呈南北向展布的规律。根据沉积相的时空展布规律,建立了本区盒8段的沉积相模式。