Ti—15—3合金超塑性拉伸变表过程的计算机优化控制

通过单片计算机对Ｔｉ－１５－３合金超塑性拉伸变表过程进行优化控制，讨论了其优化原理和控制方法，介绍了该计算机控制系统的硬件和软件。实验结果表明，超塑变表过程的优化控制能显著提高Ｔｉ－１５－３钛合金铁超美德性能，是一种有应用价值的最佳变形模式。     

应用凑合反推法建立一维非定常气流的广义变分原理

变分原理是有限元以及变分直接解法的理论基础，然而由于流体力不往往是强非线性的，因此建立变分原理是相当困难的一个难题。本文介绍了一种建立流体力学变分原理的有效方法－凑合反推法。应用该方法，作者建立了一维为截面非定常可压缩均熵流动的亚广义变分原理及广义变分原理。     

Cn系列量子群的De—Rham复形

首先介绍Ｃｎ系列量子群，并给出相应的双协变一阶微分运算。最后，给出了Ｃｎ系列量子群的Ｄｅ－Ｒｈａｍ复形。     

南海表面海温异常对南海季风影响的数值模拟

采用P-σ混合坐标系区域气候模式模拟了4－7月南海季风的爆发、演变过程，并进行了3组敏感性数值试验，研究南海表面海温异常对南海季风的影响，得到以下结论：（1）南海4月份海温异常对南海季风的爆发日期影响不大，但对季风爆发后的强度有所影响，异常增温造成南海季风增强，异常降温则南海季风减弱。（2）南海季风爆发和强度的变化与南海本身的海温变化情况有密切的关系，尤其是5月份南海海温异常。5月份南海异常增温可以使南海季风提前爆发，季风增强，南海海温异常降低时，南海季风爆发的时间推迟，季风减弱。（3）南海海温持续异常可以影响南海及中国大陆的高低空环流变化，海温持续异常增温可以使南海季风提前爆发，显地加强南海季风，并有利于南海季风向北推进，但当海温在6月份进一步持续增温时，则有利于季风维持在较南地区，阻碍季风向北发展；当海温持续异常降低时，南海季风推迟爆发，且明显减弱。     

关于Hartaman—Stampacchia变分不等式

本文论证了Ｆａｎ Ｋｙ不等式，Ｂｒｏｕｗｅｒ不动点定理，Ｈａｒｔｍａｎ－Ｓｔａｍｐａｃｃｈｉａ变分不等式在逻辑上的等价性，以及证明了Ｈ－Ｓ不等式的深化－Ｂｒｏｗｄｅｒ－Ｈａｒｔｍａｎ－Ｓｔａｍｐａｃｃｈｉａ变经不等式。     

关于Hartman-Stampacchia变分不等式

本文论证FanKy不等式，Brouwer不动点定理，Hartman－Stampacchia变分不等式在逻辑上的等价性．以及证明了H－S不等式的深化－Browder－Hartman－Stampacchia变分不等式。     

拟协调模式大变形板壳单元的变分基础

探讨了拟协调模式大变形板壳有限元的变分基础，提出了其相应的大变形板壳广义变分原 理。它不但放松了曲率－挠度关系，而且还分别放松了膜向应变－位移关系和转动分显－挠度关系。     

解非线性混合似变分不等式的预测-校正迭代算法

对映象引入了部分松驰η－强单调性概念，应用辅助变分不等式技巧，建议和分析了求解非线性混合似变分不等式的预测－校正迭代算法，算法的收敛证明仅需要映象的部分松驰η－强单调性，此性质比η－余强制性更弱，这些算法的收敛性结果 的且推广了文献中某些已知结果。     

变步长差分法求解薄板小挠度弯曲问题

本文介绍斜弯薄板弹性阶段小挠度变形的位移、应力的一种数值解法－－变步长差分法。为能较精确较快得到问题的解,文中推导了任意变步长网格划分的差分方程及边界条件,以求解薄板小挠度弯曲问题。     

拟协调元与广义变分原理

本文从修正的Ｈｅｌｌｉｎｇｅｒ－Ｒｅｉｓｓｎｅｒ变分原理出发，在一定的条件下．推出了拟协调元公式．为拟协调元提供了一种变分解释，也为建立基于Ｈｅｌｌｉｎｇｅｒ－Ｒｅｉｓｓｎｅｒ变分原理的杂交模型提供了一个新的工具。     

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.     

An X-ray-emitting blast wave from the recurrent nova RS Ophiuchi

Stellar explosions such as novae and supernovae produce most of the heavy elements in the Universe. The onset of a nova is well understood as driven by runaway thermonuclear fusion reactions on the surface of a white dwarf in a binary star system; but the structure, dynamics and mass of the ejecta are not well known. In rare cases, the white dwarf is embedded in the wind nebula of a red-giant companion, and the explosion products plough through the nebula and produce X-ray emission. Here we report X-ray observations of such an event, from the eruption of the recurrent nova RS Ophiuchi. The hard X-ray emission from RS Ophiuchi early in the eruption emanates from behind a blast wave, or outward-moving shock wave, that expanded freely for less than 2 days and then decelerated owing to interaction with the nebula. The X-rays faded rapidly, suggesting that the blast wave deviates from the standard spherical shell structure. The early onset of deceleration indicates that the ejected shell had a low mass, the white dwarf has a high mass, and that RS Ophiuchi is therefore a progenitor of the type of supernova (type Ia) integral to studies of the expansion of the Universe.     

核心坍缩超新星中心黑洞超吸积在星系尺度上的贡献

核心坍缩超新星(Core-Collapse Supernova,CCSN)是大质量恒星演化末期的爆发现象,产生了宇宙中大多数的中子星和恒星级黑洞等致密天体.爆发可能伴随着强磁场中子星或黑洞超吸积引发的剧烈长时标伽马射线暴.CCSN还被认为是宇宙重元素的主要来源之一.本综述介绍了我们近期对CCSN中心黑洞超吸积过程的系列研究成果,主要包括研究了大质量星系中心附近伽马射线暴余辉阶段,因大量暗物质粒子湮灭电子注入而引发的光变和能谱的形态变化,探讨了其作为暗物质探测手段的可能性;研究了坍缩星框架下,中微子主导吸积流外流对核合成的贡献,及对太阳临近空间、(活动)星系等化学组分和演化的影响;最后,从数值模拟角度讨论了CCSN起源的致密天体质量分布,给出了低质量间隙可能起源于CCSN爆发能量分布的结论.     

Survival of a brown dwarf after engulfment by a red giant star

Many sub-stellar companions (usually planets but also some brown dwarfs) orbit solar-type stars. These stars can engulf their sub-stellar companions when they become red giants. This interaction may explain several outstanding problems in astrophysics but it is unclear under what conditions a low mass companion will evaporate, survive the interaction unchanged or gain mass. Observational tests of models for this interaction have been hampered by a lack of positively identified remnants-that is, white dwarf stars with close, sub-stellar companions. The companion to the pre-white dwarf AA Doradus may be a brown dwarf, but the uncertain history of this star and the extreme luminosity difference between the components make it difficult to interpret the observations or to put strong constraints on the models. The magnetic white dwarf SDSS J121209.31 + 013627.7 may have a close brown dwarf companion but little is known about this binary at present. Here we report the discovery of a brown dwarf in a short period orbit around a white dwarf. The properties of both stars in this binary can be directly observed and show that the brown dwarf was engulfed by a red giant but that this had little effect on it.     

The age of the Milky Way inner halo

The Milky Way galaxy has several components, such as the bulge, disk and halo. Unravelling the assembly history of these stellar populations is often restricted because of difficulties in measuring accurate ages for low-mass, hydrogen-burning stars. Unlike these progenitors, white dwarf stars, the 'cinders' of stellar evolution, are remarkably simple objects and their fundamental properties can be measured with little ambiguity. Here I report observations of newly formed white dwarf stars in the halo of the Milky Way, and a separate analysis of archival data in the well studied 12.5-billion-year-old globular cluster Messier 4. I measure the mass distribution of the remnant stars and invert the stellar evolution process to develop a mathematical relation that links this final stellar mass to the mass of their immediate progenitors, and therefore to the age of the parent population. By applying this technique to a small sample of four nearby and kinematically confirmed halo white dwarf stars, I calculate the age of local field halo stars to be 11.4?±?0.7 billion years. The oldest globular clusters formed 13.5?billion years ago. Future observations of newly formed white dwarf stars in the halo could be used to reduce the uncertainty, and to probe relative differences between the formation times of the youngest globular clusters and the inner halo.     

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.     

A class of compact dwarf galaxies from disruptive processes in galaxy clusters

Dwarf galaxies have attracted increased attention in recent years, because of their susceptibility to galaxy transformation processes within rich galaxy clusters. Direct evidence for these processes, however, has been difficult to obtain, with a small number of diffuse light trails and intra-cluster stars being the only signs of galaxy disruption. Furthermore, our current knowledge of dwarf galaxy populations may be very incomplete, because traditional galaxy surveys are insensitive to extremely diffuse or compact galaxies. Aware of these concerns, we recently undertook an all-object survey of the Fornax galaxy cluster. This revealed a new population of compact members, overlooked in previous conventional surveys. Here we demonstrate that these 'ultra-compact' dwarf galaxies are structurally and dynamically distinct from both globular star clusters and known types of dwarf galaxy, and thus represent a new class of dwarf galaxy. Our data are consistent with the interpretation that these are the remnant nuclei of disrupted dwarf galaxies, making them an easily observed tracer of galaxy disruption.     

性连锁矮小型基因对黄羽肉鸡早期生长的影响

利用矮小型黄羽肉鸡品系和３个正常型黄羽肉鸡品系及其杂交鸡为材料，测定早期生长体重，研究ｄｗ基因对黄羽肉鸡早期生长的影响。结果表明，ｄｗ基因严重阻碍黄羽肉鸡生长速度，对正常体型基因Ｄｗ为不完全隐性。矮小型品系母鸡与两个非同源正常型公鸡杂交，其杂交后代体重表现出显著的杂交优势，但其杂交优势率因正常型品系类型不同而有差异，轻型品系杂交效果优于重型品系。     

An energetic stellar outburst accompanied by circumstellar light echoes

Some classes of stars, including novae and supernovae, undergo explosive outbursts that eject stellar material into space. In 2002, the previously unknown variable star V838 Monocerotis brightened suddenly by a factor of approximately 10(4). Unlike a supernova or nova, it did not explosively eject its outer layers; rather, it simply expanded to become a cool supergiant with a moderate-velocity stellar wind. Superluminal light echoes were discovered as light from the outburst propagated into the surrounding, pre-existing circumstellar dust. Here we report high-resolution imaging and polarimetry of those light echoes, which allow us to set direct geometric distance limits to the object. At a distance of >6 kpc, V838 Mon at its maximum brightness was temporarily the brightest star in the Milky Way. The presence of the circumstellar dust implies that previous eruptions have occurred, and spectra show it to be a binary system. When combined with the high luminosity and unusual outburst behaviour, these characteristics indicate that V838 Mon represents a hitherto unknown type of stellar outburst, for which we have no completely satisfactory physical explanation.     

5种地被竹光合日变化特性研究

以菲白竹、黄条金刚竹、鹅毛竹、铺地竹和菲黄竹5种地被竹为试材进行盆栽试验,测定其光合日变化。试验结果表明：5种地被竹净光合速率和蒸腾速率日变化均为双峰曲线,具有典型的“午休”特征。各环境因子主要通过对光合有效辐射、水压亏缺、胞间CO2浓度和叶面温度的作用而影响的净光合速率,气孔导度对光合特征参数的变化影响最大,且对净光合速率起决定性作用,是影响光合的限制因子。光合“午休”是由于气孔导度的降低,主要受气孔因素限制。