An asymmetric shock wave in the 2006 outburst of the recurrent nova RS Ophiuchi

Nova outbursts take place in binary star systems comprising a white dwarf and either a low-mass Sun-like star or, as in the case of the recurrent nova RS Ophiuchi, a red giant. Although the cause of these outbursts is known to be thermonuclear explosion of matter transferred from the companion onto the surface of the white dwarf, models of the previous (1985) outburst of RS Ophiuchi failed to adequately fit the X-ray evolution and there was controversy over a single-epoch high-resolution radio image, which suggested that the remnant was bipolar rather than spherical as modelled. Here we report the detection of spatially resolved structure in RS Ophiuchi from two weeks after its 12 February 2006 outburst. We track an expanding shock wave as it sweeps through the red giant wind, producing a remnant similar to that of a type II supernova but evolving over months rather than millennia. As in supernova remnants, the radio emission is non-thermal (synchrotron emission), but asymmetries and multiple emission components clearly demonstrate that contrary to the assumptions of spherical symmetry in models of the 1985 explosion, the ejection is jet-like, collimated by the central binary whose orientation on the sky can be determined from these observations.     

An ancient nova shell around the dwarf nova Z Camelopardalis

Cataclysmic variables (classical novae and dwarf novae) are binary star systems in which a red dwarf transfers hydrogen-rich matter, by way of an accretion disk, to its white dwarf companion. In dwarf novae, an instability is believed to episodically dump much of the accretion disk onto the white dwarf. The liberation of gravitational potential energy then brightens these systems by up to 100-fold every few weeks or months. Thermonuclear-powered eruptions thousands of times more luminous occur in classical novae, accompanied by significant mass ejection and formation of clearly visible shells from the ejected material. Theory predicts that the white dwarfs in all dwarf novae must eventually accrete enough mass to undergo classical nova eruptions. Here we report a shell, an order of magnitude more extended than those detected around many classical novae, surrounding the prototypical dwarf nova Z Camelopardalis. The derived shell mass matches that of classical novae, and is inconsistent with the mass expected from a dwarf nova wind or a planetary nebula. The shell observationally links the prototypical dwarf nova Z Camelopardalis with an ancient nova eruption and the classical nova process.     

A blast wave from the 1843 eruption of eta Carinae

Very massive stars shed much of their mass in violent precursor eruptions as luminous blue variables (LBVs) before reaching their most likely end as supernovae, but the cause of LBV eruptions is unknown. The nineteenth-century eruption of eta Carinae, the prototype of these events, ejected about 12 solar masses at speeds of 650 km s(-1), with a kinetic energy of almost 10(50) erg (ref. 4). Some faster material with speeds up to 1,000-2,000 km s(-1) had previously been reported but its full distribution was unknown. Here I report observations of much faster material with speeds up to 3,500-6,000 km s(-1), reaching farther from the star than the fastest material in previous reports. This fast material roughly doubles the kinetic energy of the nineteenth-century event and suggests that it released a blast wave now propagating ahead of the massive ejecta. As a result, eta Carinae's outer shell now mimics a low-energy supernova remnant. The eruption has usually been discussed in terms of an extreme wind driven by the star's luminosity, but the fast material reported here indicates that it may have been powered by a deep-seated explosion rivalling a supernova, perhaps triggered by the pulsational pair instability. This may alter interpretations of similar events seen in other galaxies.     

中心内爆引起的圆柱壳流固耦合问题数值模拟

针对中心装药的冲击波加载,研究了椭球封头圆柱壳的流固耦合问题.基于法向位移、速度和力建立流固界面边界条件,采用FVM求解积分ALE型无粘流体力学方程组,采用FEM求解虚功原理,得到内爆流场冲击波和壳体应力波的传播过程.结果表明:我们的方法和计算软件可研究内爆引起的壳体流固耦合问题.尽管壳体结构和装药位置相对简单,但冲击波在壳内传播和内壁面多次反射产生的波系结构相当复杂,压力云图刻画了冲击波演化图像.壳体所受加载特征是:前期表现为冲击波超压,后期表现为冲量,壳体变形依赖冲击波加载历史.封头顶点、封头和侧壁交线以及距中心最近的中环面出现较大等效应力,也是结构易破坏的部位.     

坑道截面形状对化爆冲击波传播规律的影响程度分析

为了弄清坑道截面形状对化爆冲击波传播规律的影响,采用LSDYNA动力有限元软件对不同形状坑道内化爆冲击波的传播过程进行数值模拟和对比分析.研究表明:采用合理的有限元模型可以有效地模拟坑道中化爆冲击波的传播过程;化爆冲击波在不同截面形状坑道内的衰减规律基本一致,但冲击波超压峰值有显著差异;圆形坑道内化爆冲击波超压峰值最低,是直墙圆拱形坑道内的60%左右,正方形坑道内超压峰值最高,是直墙圆拱形坑道内的300%左右;工程设计时,必须考虑坑道截面形状对冲击波的影响,宜尽量采用圆形坑道.     

从散射波函数方法中导出的非平衡格林函数公式

给出了从Landauer-Buttiker's 散射波函数导出无相互作用介观系统中的非平衡格林函数公式的严格证明.结果表明:尽管散射波函数理论和非平衡格林函数理论基于非常不同的物理思想,但在应用上这2个等价的理论工具是可以互补的.     

压力容器爆炸时抛出物能量的百分比计算及冲击波的破坏范围估计

针对１９９９年５月３日苏州合成化工厂精制釜发生爆炸的实际情况,计算抛出物占爆炸总能量的百分比及所产生冲击波的破坏范围估计。     

Kelvin-Helmholtz instabilities as the source of inhomogeneous mixing in nova explosions

Classical novae are thermonuclear explosions in binary stellar systems containing a white dwarf accreting material from a close companion star. They repeatedly eject 10(-4)-10(-5) solar masses of nucleosynthetically enriched gas into the interstellar medium, recurring on intervals of decades to tens of millennia. They are probably the main sources of Galactic (15)N, (17)O and (13)C. The origin of the large enhancements and inhomogeneous distribution of these species observed in high-resolution spectra of ejected nova shells has, however, remained unexplained for almost half a century. Several mechanisms, including mixing by diffusion, shear or resonant gravity waves, have been proposed in the framework of one-dimensional or two-dimensional simulations, but none has hitherto proven successful because convective mixing can only be modelled accurately in three dimensions. Here we report the results of a three-dimensional nuclear-hydrodynamic simulation of mixing at the core-envelope interface during nova outbursts. We show that buoyant fingering drives vortices from the Kelvin-Helmholtz instability, which inevitably enriches the accreted envelope with material from the outer white-dwarf core. Such mixing also naturally produces large-scale chemical inhomogeneities. Both the metallicity enhancement and the intrinsic dispersions in the abundances are consistent with the observed values.     

利用RS和GIS技术对南大港湿地类型的调查研究

以南大港湿地2000年6月陆地卫星多波段遥感影像为主要研究资料,建立湿地分类系统和解译标志。利用遥感和地理信息系统技术相结合对南大港湿地资源现状进行类型分布和面积调查。     

超声旋转行波马达研究

采用解析法求解了环形行波超声马达定子振动的幅频特性，并在此基础上，依据马达转子的动力学方程，建立了定子与转子间的接触数学模型，从理论和实验两个方面分析了输入激励电源频率及电压大小变化对马达输出机械特性的影响，结果表明，超声马达的输出特性与激励电源的参数密切相关，在谐振频率附近，马达的阻转力矩和输出转速都有较大增加，增加驱动电压，阻转力矩和输出转速将单调增大。     

高炉煤气洗涤废水治理技术研究现状

高炉煤气洗涤废水是我国钢铁企业的主要工业废水之一,高炉煤气洗涤废水的排放不仅是一种资源浪费,而且对环境的污染也非常严重．综述国内外有关高炉煤气洗涤废水的治理方法,可以对高炉煤气洗涤废水的处理起到一定参考作用,在保护钢铁企业周围生态环境的同时,提高水资源的利用率．     

富硼高炉渣中遂安石相的析出行为

利用扫描电镜和X射线衍射分析研究了富硼渣Mgo-B2O3-SiO2-Al2O3-CaO渣系在不同冷却速率下,连续冷却和分段冷却时富硼渣中遂安石相的析出行为.试验结果表明,熔渣以不同的冷却速率由1 500℃冷却到800 ℃时,由于富硼炉渣中高熔点的镁橄榄石相先于遂安石相析出,对遂安石相的析出起到阻碍作用.采用分段冷却的方...     

椭圆极化电磁波在界面的极化分析

运用波的极化概念,将入射的椭圆极化电磁波分解为互相正交的2个直线极化波,利用边界条件的匹配分别讨论它们与界面的作用结果,再进行合成;并就椭圆极化电磁波在界面垂直入射,以布儒斯特角入射及在界面发生全反射时的极化规律进行了分析.     

Influence of CeO_2 addition on the preparation of foamed glass-ceramics from high-titanium blast furnace slag

Foamed glass-ceramics doped with cerium oxide(CeO_2)were successfully prepared from high-titanium blast furnace slag by one-step sintering.The influence of CeO_2 addition(1.5wt%–3.5wt%)on the crystalline phases,microstructure,and properties of foamed glass-ceramics was studied.Results show that CeO_2 improves the stability of the glass phase and changes the two-dimensional crystallization mechanism into three-dimensional one.XRD analysis indicates the presence of Ca(Mg,Fe)Si_2O_6 and Ca(Ti,Mg,Al)(Si,Al)_2O_(6 )in all sintered samples.Added with CeO_2,Ti CeO_4 precipitates,and crystallinity increases,leading to increased thickness of pore walls and uniform pores.The comprehensive properties of foamed glass-ceramics are better than that of samples without CeO_2.In particular,the sample added with a suitable amount of CeO_2(2.5wt%)exhibits bulk density that is similar to and compressive strength(14.9 MPa)that is more than twice of foamed glass-ceramics without CeO_2.     

Equal Width波方程的精确行波解与波的动态模拟

继Abdulkadir Dogan用Galar方法求解Equal Width波方程得到一些数值解之后,我们利用动力系统分支理论再次求解了这个方程.确定了存在光滑的孤立波和周期波解的参数条件.给出了一些精确的解析行波解.同时,给出了这些行波解的动态模拟图.     

RS-485总线系统可靠性分析

介绍了基于RS-485总线系统的常见故障与问题,分析了产生的原因并给出了提高RS-485总线系统可靠性的方法。     

超声法提取金鸡纳生物碱的工艺

研究金鸡纳总生物碱的超声提取工艺.采用L9(34)正交设计通过正交试验得出了超声提取的最佳工艺条件.超声提取的影响因素顺序为提取次数＞提取时间＞料液比,其最佳提取条件为A2B2C2,即8倍量的甲苯提取液提取4次,每次45 min.实验证明该提取工艺方法经济合理.     

Outer-core compositional stratification from observed core wave speed profiles

Light elements must be present in the nearly pure iron core of the Earth to match the remotely observed properties of the outer and inner cores. Crystallization of the inner core excludes light elements from the solid, concentrating them in liquid near the inner-core boundary that potentially rises and collects at the top of the core, and this may have a seismically observable signal. Here we present array-based observations of seismic waves sensitive to this part of the core whose wave speeds require there to be radial compositional variation in the topmost 300?km of the outer core. The velocity profile significantly departs from that of compression of a homogeneous liquid. Total light-element enrichment is up to five weight per cent at the top of the core if modelled in the Fe-O-S system. The stratification suggests the existence of a subadiabatic temperature gradient at the top of the outer core.