Infrared diffuse interstellar bands in the Galactic Centre region

The spectrum of any star viewed through a sufficient quantity of diffuse interstellar material reveals a number of absorption features collectively called 'diffuse interstellar bands' (DIBs). The first DIBs were reported about 90 years ago, and currently well over 500 are known. None of them has been convincingly identified with any specific element or molecule, although recent studies suggest that the DIB carriers are polyatomic molecules containing carbon. Most of the DIBs currently known are at visible and very near-infrared wavelengths, with only two previously known at wavelengths beyond one micrometre (10,000 ?ngstr?ms), the longer of which is at 1.318?micrometres (ref. 6). Here we report 13 diffuse interstellar bands in the 1.5-1.8 micrometre interval on high-extinction sightlines towards stars in the Galactic Centre. We argue that they originate almost entirely in the Galactic Centre region, a considerably warmer and harsher environment than where DIBs have been observed previously. The relative strengths of these DIBs towards the Galactic Centre and the Cygnus OB2 diffuse cloud are consistent with their strengths scaling mainly with the extinction by diffuse material.     

对激波的讨论

本文讨论了激波的形成过程 ,给出了相应的数学推导 ,并求出激波在理想气体绝热过程中的传播速度。     

爆破空气冲击波及其预防

工程爆破时所产生的爆破振动、爆破空气冲击波、爆破噪音以及爆破飞石和毒气是公认的爆破公害，亦是公安机关治安管理部门最为关注的焦点问题之一。本文对爆破空气冲击波危害、安全距离进行了初步研究，在此基础上提出了削弱爆破冲击波公害发生的基本措施。     

A magnetic torsional wave near the Galactic Centre traced by a 'double helix' nebula

The magnetic field in the central few hundred parsecs of the Milky Way has a dipolar geometry and is substantially stronger than elsewhere in the Galaxy, with estimates ranging up to a milligauss (refs 1-6). Characterization of the magnetic field at the Galactic Centre is important because it can affect the orbits of molecular clouds by exerting a drag on them, inhibit star formation, and could guide a wind of hot gas or cosmic rays away from the central region. Here we report observations of an infrared nebula having the morphology of an intertwined double helix about 100 parsecs from the Galaxy's dynamical centre, with its axis oriented perpendicular to the Galactic plane. The observed segment is about 25 parsecs in length, and contains about 1.25 full turns of each of the two continuous, helically wound strands. We interpret this feature as a torsional Alfvén wave propagating vertically away from the Galactic disk, driven by rotation of the magnetized circumnuclear gas disk. The direct connection between the circumnuclear disk and the double helix is ambiguous, but the images show a possible meandering channel that warrants further investigation.     

弹片与爆炸冲击波耦合作用分析

弹片和冲击波是武器战斗部毁伤效应的两个重要方面,两者具有一定的相关性.通过研究弹片与爆炸冲击波的耦合作用,分析并推导了弹片在空气中的运动规律和运动方程,以及弹壳对武器爆炸冲击波的影响.通过实例分析,验证了建立的模型和计算方法的合理性和正确性.弹片的最大速度和壳体厚度对爆炸冲击波能量的影响因子随着弹壳厚度的增加而降低.弹壳增厚会导致在爆轰气体与弹壳相互作用的阶段,有更多的能量损耗于壳体膨胀和破碎过程,从而使爆炸冲击波的能量减弱.在实际计算中,必须考虑弹壳的存在以及壳体厚度对爆炸冲击波能量的影响作用.     

激波-多涡列-声场相互作用及其POD分析

采用5阶WENO格式,通过数值求解二维非定常欧拉方程,模拟了激波与四涡组成的涡列的相互作用过程.通过研究马赫数为1.05的激波与强度为0.25的多涡列相互作用,进一步揭示了激波-涡列相互作用的动力学特性以及声波的产生过程.     

保守场的一类特殊激波解

文章研究了一类消失项为εxxu ε2τ1 xxtu ε2τ2 xxxu时非凸保守场方程的激波解(弱解),通过构造行波的方法得到了近似方程行波解存在的必要条件,并讨论了该行波解的若干性质。证明了该行波解u(x,t,ε)的极限(ε→ 0)就是保守场方程的弱解,并利用行波来构造该非凸保守场方程的激波解。     

球形装药水下爆炸初始冲击波能量计算

文中运用流体动力学理论,水中冲击波理论,对某些工业炸药和单质炸药水下爆炸后爆炸气体产物与水交界面初始冲击波参数及初始冲击波能量进行了计算.计算结果可为炸药水下爆炸总能量提供依据.     

爆炸应力波在SRC柱中传播特性

钢骨混凝土(SRC)柱由于钢骨的存在,与钢柱和混凝土柱有明显的不同.以理论分析和计算机模拟相结合的方法,分析了爆炸冲击波在SRC柱中的传播特征,重点研究了爆炸冲击波在SRC柱支座截面和跨中截面的传播特点以及钢骨的存在对爆炸冲击波传播特征的影响.在跨中附近,可以用平面应力波理论分析爆炸冲击波在SRC柱中的传播;在支座附近,必须用空间波动理论研究爆炸冲击波在SRC柱中的传播.钢骨的存在造成爆炸冲击波在SRC柱中的传播路径非常复杂;钢骨的存在可以导致钢骨翼缘外侧的混凝土内冲击应力增大,但是可以减小钢骨翼缘内侧混凝土内的冲击应力,从而起到保护钢骨翼缘内侧混凝土的作用.     

激波诱导的层流边界层方程的近似解析解

研究了由激波诱导的边界层问题,利用Adomian解析分解方法对不同速度比例参数给出了问题的级数形式的近似解析解和相应的壁摩擦因数近似值,该近似解析解具有快速收敛性和易于计算性。最后对近似解所推出结果和所得壁摩擦因数与文献中的数值解进行了比较验证,证实了提出的解析近似方法的准确性和可靠性,所提出的思想方法还可用于解决其它科学和工程技术问题。     

The experimental study of interaction between shock wave and turbulence

The interaction between shock wave and turbulence has been studied in supersonic turbulent mix layer wind tunnel. The interaction between oblique shock wave and turbulent boundary layer and the influence of large vortex in mix layer on oblique shock wave have been observed by NPLS technique. From NPLS image, not only complex flow structure is observed but also time-dependent supersonic flow visualization is realized. The mechanism of interaction between shock wave and turbulence is discussed based on high quality NPLS image.     

Study of interaction between shock wave and unsteady boundary layer

This paper reports theoretical and experimental study of a new type of interaction of a moving shock wave with an unsteady boundary layer. This type of shock wave-boundary layer interaction describes a moving shock wave interaction with an unsteady boundary layer induced by another shock wave and a rarefaction wave. So it is different from the interaction of a stationary shock wave with steady boundary layer, also different from the interaction of a reflected moving shock wave at the end of a shock tube with unsteady boundary layer induced by an incident shock. Geometrical shock dynamics is used for the theoretical analysis of the shock wave-unsteady boundary layer interaction, and a double-driver shock tube with a rarefaction wave bursting diaphragm is used for the experimental investigation in this work.     

星际介质中的纳米尘埃

星际尘埃,作为一种在宇宙中普遍存在的重要成分,在天文学研究中起着重要的作用.星际介质中的尘埃其尺寸分布涵盖从几个埃到几个亚微米的范围.对于有这样大的尺寸差异的星际尘埃,尘埃的热辐射机制差别很大.较大的尘埃颗粒,有比较大的吸收和发射截面,因而其吸收光子的速率和发射的速率也比较大,可以从吸收和发射能量的平衡来得出热平衡温度,并用热平衡温度和黑体辐射来计算其光谱.对于大小为纳米尺度或者更小的尘埃,由于其很小的尺寸,这类尘埃的热容量非常小.当这种尘埃吸收一个与其热容量相当或者更大能量光子的时候,尘埃就会经历一个非常明显的温度涨落:尘埃吸收一个紫外光子瞬间,其温度迅速上升,到达顶点后,由于尚没有外来能量的影响(因吸收截面小,吸收光子几率也非常小),尘埃开始通过热辐射降温,直到吸收另一个光子开始新的循环,这就是单光子加热模型(Single-Photon Heating Model).显然,热平衡和单光子加热是两个明显不同的过程.对于单光子加热,由于尘埃颗粒的温度涨落作用,尘埃不会处于一个稳定的平衡温度状态,因而不能用单一温度来描述其热辐射,必须计算出尘埃在温度涨落过程中的温度分布函数,然后计算其辐射谱.本文主要介绍纳米颗粒在星际空间中的存在证据,单光子加热模型,以及处于温度涨落中纳米颗粒的辐射特征.     

冲击作用下多孔材料热力学特征的模拟与分析

强冲击波的作用可在多孔材料中诱发复杂的时空耗散过程,在这期间系统整体处于远离平衡的状态,对这一过程的稳定模拟和结果分析均具有较强的挑战性。使用近期针对超高速碰撞而发展起来的物质点方法对这一过程进行模拟,引入积分几何和数值图像处理中的形态学描述来处理和分析系统热力学特征量例如温度的Turing斑图, 揭示出3个Minkowski泛函(白色区域相对面积、边界总长度、欧拉特征量)与系统中“高温区”所占份额、“热点”在空间的分布方式之间的对应,揭示出Minkowski泛函演化特征与冲击波及多孔材料相互作用过程之间的对应。研究了孔隙度和冲击波强度对物质状态参量的影响。     

爆炸应力波对深埋巷道的作用效应分析

运用工程分析软件ANSYS模拟几种常见形状的巷道结构在爆炸应力波作用下围岩的位移时间历程和Mises等效应力时间历程,进而分析这些不同形状巷道结构在爆炸应力波作用下的位移、振动、变形情况,得出在爆炸应力波作用下巷道结构易破坏的位置并给出防护对策。     

基于激光冲击波的金属板料精密校形技术

为了解决金属板料在装配过程中经常发生变形而产生装配困难的问题,尤其大型或超大型结构件的变形问题,在分析传统校形方法特点的基础上,提出一种基于激光冲击波诱导残余应力的金属板料校形技术.对激光冲击波金属板料校形系统的组成、工作原理进行了阐述.以NA:YAG激光器为基础构建校形试验系统,对0.6 mm厚的金属铝板的进行了校直...     

自动机喷管激波的时空衍变仿真与验证

自动机喷管不同的结构形式对后坐冲击的对冲效率是不同的,为了获得更好的喷管激波消减后坐冲击的方案,构建了不同结构的喷管模型;利用燃气可压缩雷诺平均纳维-斯托克斯(N-S)方程,对不同结构的激波时空衍变的过程进行仿真,得出流场图谱、火药气体载荷分布;方案1和方案2的喷管设计参数:锥度均为12°,长度分别为360、380 m...