Magnetic and optical spiral arms in the galaxy NGC 6946

The spiral pattern in the nearby spiral galaxy NGC 6946 has been studied using the wavelet transformation technique, applied to galaxy images in polarized and total non-thermal radio emission at λλ 3.5 and 6.2 cm, in broadband red light, in the λ 21.1 cm H  i line and in the optical Hα line. Well-defined, continuous spiral arms are visible in polarized radio emission and red light, where we can isolate a multi-armed pattern in the range of galactocentric distances 1.5–12 kpc, consisting of four long arms and one short spiral segment. The 'magnetic arms' (visible in polarized radio emission) are localized almost precisely between the optical arms. Each magnetic arm is similar in length and pitch angle to the preceding optical arm (in the sense of galactic rotation) and can be regarded as its phase-shifted image. Even details like a bifurcation of an optical arm have their phase-shifted counterparts in the magnetic arms. The average relative amplitude of the optical spiral arms (the stellar density excess over the azimuthal average) grows with galactocentric radius up to 0.3–0.7 at r ≃5 kpc, decreases by a factor of two at r =5–6 kpc and remains low at 0.2–0.3 in the outer parts of the galaxy. By contrast, the magnetic arms have a constant average relative amplitude (the excess in the regular magnetic field strength over the azimuthal average) of 0.3–0.6 in a wide radial range r =1.5–12 kpc. We briefly discuss implications of our findings for theories of galactic magnetic fields.     

A stochastic Monte Carlo approach to model real star cluster evolution – II. Self-consistent models and primordial binaries

The new approach outlined in Paper I to follow the individual formation and evolution of binaries in an evolving, equal point-mass star cluster is extended for the self-consistent treatment of relaxation and close three- and four-body encounters for many binaries (typically a few per cent of the initial number of stars in the cluster mass). The distribution of single stars is treated as a conducting gas sphere with a standard anisotropic gaseous model. A Monte Carlo technique is used to model the motion of binaries, their formation and subsequent hardening by close encounters, and their relaxation (dynamical friction) with single stars and other binaries. The results are a further approach towards a realistic model of globular clusters with primordial binaries without using special hardware. We present, as our main result, the self-consistent evolution of a cluster consisting of 300 000 equal point-mass stars, plus 30 000 equal-mass binaries over several hundred half-mass relaxation times, well into the phase where most of the binaries have been dissolved and evacuated from the core. The cluster evolution is about three times slower than found by Gao et al. Other features are rather comparable. At every moment we are able to show the individual distribution of binaries in the cluster.     

The evolution of bodies orbiting in the trans-Neptunian region on to intermediate-type orbits

We investigate the dynamical evolution of 210 hypothetical massless bodies initially situated between 10 and 30 au from the Sun in order to determine the general characteristics of the evolved system. This is of particular relevance to the understanding of the origin of Edgeworth–Kuiper belt objects on scattered intermediate orbits, such as 1996 TL ₆₆, which have high eccentricity and semimajor axis but nevertheless have perihelion in the region between 30 and 50 au from the Sun.     

景观生态学与生物圈保护区———1997年选择性诺贝尔奖获得者德国Greifs wald大学景观生态学家Prof.Dr.Michael Succow先生2000年6月北京-新疆访问考察记行

介绍了苏考吾教授以及他在北京和新疆访问考察与报告的主要科学内容、选择性诺贝尔奖、德国景观生态学发展简史、联合国教科文组织生物圈保护区和新疆现状     

高速远程崩滑动力学的研究现状及发展趋势

高速远程崩滑动力学机理的研究,一直是国内外工程地质与山地灾害领域崩塌、滑坡灾害研究的前沿热点问题。对这一研究领域,最近几十年来所取得的研究成果、研究现状及发展趋势进行了述评。厘定了高速远程崩滑的定义;详细地阐述了国内外众多典型重大高速远程崩滑灾害事件的几何学、运动学特征;概述了迄今为止所提出的高速远程崩滑形成的各种动力学机理;分析与讨论了高速远程崩滑动力学机理研究的发展趋势与动向;提出了今后进一步研究的总体思路、目标与应重点解决的关键问题。     

薄分子云湍流结构函数的倾角改正及其应用

通过结构函数可以测量湍流的能量级联速率.在实际观测中,无法测量分子云中气体的3维速度,这使得其湍流结构函数难以测量.对垂直于视线方向的薄分子云的情形,结构函数Stt2可以通过云核速度弥散(core velocity dispersion,CVD)进行测量,CVD2=1/2Stt2.对此进行推广,对于不垂直于视线方向的薄分子云,CVD2=1/2Stt2(1-1/8cos2θ)R2/3,其中,θ是视线方向与投影方向的夹角,平均投影距离与3维距离之比R可以用第2类椭圆积分E(k,φ)表示为R=2/πE(cosθ,π/2).     

烟台芝罘湾底质沉积物粒度特征和沉积动力环境研究

根据芝罘湾海域110个底质沉积物样品粒度分析结果,对沉积物类型和粒度参数分布进行了总结。在此基础上,利用粒径趋势分析模型(GSTA)和沉积动力判别图解,探讨了底质沉积物的运移趋势及沉积水动力规律。研究表明,芝罘湾海域底质沉积物类型共有8种,其中砂质泥、砂质粉砂、泥和粉砂分布最广泛;平均粒径值具有从岸向海逐渐增大的趋势,分选性、偏度和峰度分别为差、正偏—极正偏、平坦—中等的特征;粒度运移趋势分析反映出套子湾泥沙向西、西南运移,芝罘湾及以东海域泥沙呈顺时针方向运移;沉积动力判别图解揭示出芝罘湾海域沉积水动力具有整体较弱的特征。     

PS测井在机场隧道地基勘查中的应用

PS测井技术是地震勘探方法之一,也是一种简便、快速、准确的原位测试技术。该文介绍了单孔法PS测井的原理及其在铁路工程勘察中的应用,主要包括根据等效剪切波,进行建筑抗震场地类别划分,铁路工程抗震场地类别划分。根据岩土动力学参数,达到评价岩体质量和划分围岩类别目的,利用剪切波速法估算岩土的承载力基本值。通过青岛机场隧道场地的工程实例说明了PS测井技术在岩土工程勘察设计中的应用情况及应用效果。     

基于计算流体力学的寒区土壤水热耦合模型研究

土壤水文过程(水分运移和传热)及其对气候变化的响应是寒区水文学的前沿问题.然而,冻土的存在使得寒区土壤水文过程变得极其复杂.此外,寒区自然环境恶劣,较难获取长时间序列和高分辨率的野外观测资料.近年来,充分利用已有的观测数据,构建寒区土壤水热耦合模型,并开展相应的数值模拟研究,已成为理解寒区土壤水文物理过程,揭示其动力学...