The initial mass function and history of the star-formation rate in star-forming complexes in galaxies

The positions of star-forming complexes (SFCs) in color-luminosity, color-color, and chemical composition-luminosity diagrams are determined by the star-formation regime (history). Taking into account the fraction of Lyman continuum photons that are not absorbed by hydrogen, we find a strong correlation between the observed color indices and the total Lyman continuum flux from the stars in SFCs. The distribution of extragalactic SFCs in a plot of the slope of the initial mass function (IMF) versus the density of stars cannot be distinguished from this distribution for clusters in the Galaxy and the Large Magellanic Cloud, where the IMF slopes were derived directly from star counts.     

Numerical simulations of the initial mass function and star-formation history using a grid of evolutionary models for star clusters

Numerical simulations are used to investigate the possibility of determining the physical properties of young star-forming complexes by finding the global minimum of a so-called deviation functional, which assigns each evolutionary model for a stellar population a number characterizing the deviation of the observed photometric properties from their model values. The deviation functional is calculated using a grid of evolutionary models computed at the Institute of Astronomy of the Russian Academy of Sciences. The parameters of the initial mass function (IMF) and the age corresponding to the global minimum of the deviation functional are strongly correlated with the IMF and age of the test model. The accuracy of the parameters of the IMF and the age are related to the random errors of the colors of the test models and the number of input parameters. A special series of numerical simulations is used to demonstrate the possibility of using the deviation functional to determine the interstellar extinction and the fraction of Lyman photons that do not contribute to the ionization of gas in a star-forming complex. The simulation results can be used to assess the accuracy of the IMF parameters and ages of young star-forming complexes based on the observational data available.     

A catalog of star-forming regions in the galaxy

This Catalog of Star-Forming Regions in the Galaxy contains coordinates and fluxes of young objects in the radio and infrared, as well as data on the radial velocities of recombination and molecular lines, for more than three thousand star-forming regions. In addition to photometric and kinematic data, we present information on diffuse and reflecting nebulae, dark and molecular clouds, and other objects related to young stars. The catalog consists of two parts. The main catalog lists star-forming regions in order of Galactic longitude and is supplemented by analogous information for star-forming regions in complexes of dark clouds with large angular sizes that are closest to the Sun. The main catalog is located at http://www.strasbg.-u.fr/pub/cats. In our preliminary study of the catalog data using a formal classification of the star-forming regions, we subdivided these objects into several classes and characterized them as being populated primarily by massive or low-mass stars at early or late stages of the star-formation process. We also distinguish between relatively nearby and distant complexes.     

Expulsion of dust from dark-matter halos at high redshifts

The conditions required for the expulsion of dust grains from primordial galaxies (dark-matter halos) are considered. The initial configuration is taken to be a dark-matter halo with the profile of a modified isothermal sphere; the baryons are taken to be in equilibrium with the corresponding virial temperature. The baryon density profile is calculated assuming hydrostatic equilibrium. A star-formation rate corresponding to a star-forming efficiency of 10% is assumed. The dust is transported from the galaxy by the radiation of stars concentrated in the central regions. Due to friction via collisions with gas in central regions, a fairly high luminosity is required in order for the radiation pressure to be strong enough to expel dust from the galaxy—the ratio of the luminosity to the total mass of the galaxy can reach unity.     

Problems of star-formation theory and prospects for submillimeter observations

We consider the current state of star-formation theory and requirements for millimeter and submillimeter observations that would enable the resolution of the most pressing problems in the physics of star formation. Two key features of star-forming regions that define these observational requirements are the relatively low energy of processes taking place there and the smallness of the corresponding spatial scales. This is especially true for objects in the latest stages of “pre-stellar” evolution, that is, hot cores, hypercompact and ultracompact HII regions, and protoplanetary disks. The angular resolution, sensitivity, and spectral coverage in existing ground-based and space submillimeter and millimeter telescopes are not fully adequate to the observtional requirements. To obtain detailed information on star-forming regions, as well as individual protostars, it is necessary to use a space-based interferometer.     

非线性破坏准则下的边坡稳定塑性极限分析

利用塑性分析上限定理,考虑岩土介质本身的非线性破坏准则,对各种不同破裂面边坡稳定性分析进行研究。针对破坏边坡破裂面不同,采用外切直线法来分析其上限解,推导出非线性破坏准则下的边坡稳定性系数计算公式,并对较复杂的对数螺旋线破裂面边坡提出初始切线法,较好地求出塑性极限分析上限解。将在非线性破坏准则下按对数螺旋线破裂面推导出的塑性极限分析上限解运用于实际边坡工程,其结果与精确塑性分析结果非常接近,为非线性破坏准则下的边坡稳定塑性极限分析提供了一条新的思路与方法。     

层状边坡岩体的屈曲和溃屈性态研究

在对层状边坡岩体结构进行稳定性分析的过程中,屈曲和溃屈是两个主要问题。针对边坡岩体结构的赋存特点和分岔特性,以及研究方法仅采用线性理论和已有研究成果只停留在结构屈曲层面上的状况,文章应用初始后屈曲理论和突变理论探讨了岩体结构的屈曲性态和溃屈性态,给出了边坡岩体上部滑动段滑动的条件,得出了边坡岩体的分岔方程和溃屈方程,指出了分岔方程的适用条件和溃屈方程的适用范围,确定了边坡岩体后屈曲状态下溃屈破坏的下限,建立了岩体结构溃屈破坏的判据,并以雅砻江下游的霸王山边坡为例进行研究。结果表明:边坡岩体的赋存状况决定了其势函数的分岔集,从边坡的分岔集可衍生出结构在分岔状态下的分岔载荷和分岔方程;分岔方程表达了边坡岩体结构的屈曲状态,也表达了结构出现屈曲的准则;边坡岩体的赋存状况还决定了岩体结构溃屈破坏时岩体材料屈服的取值范围,而岩体结构溃屈破坏的上限或下限则取决于岩体材料的屈服极限。     

Comparison of <Emphasis Type="Italic">U BV R</Emphasis> photometry of giant HII regions in the galaxy NGC 628 with a detailed grid of evolutionary models for star clusters

We present the results of U BV RI CCD photometry of giant HII regions in the spiral galaxy NGC 628, acquired with the 1.5 m telescope of the Mt. Maidanak Observatory (Uzbekistan) with an angular resolution better than 1″. We estimate the ages and interstellar extinctions of these regions and identify the acting star-formation mode by comparing the observed color indices with a detailed grid of evolutionary models covering the entire range of parameters of the initial mass function and of ages of the young star-formation complexes, and taking into account two star-formation modes. We find a radial gradient of the interstellar extinction in NGC 628, which is consistent with the radial abundance gradient found earlier by other authors from independent spectrophotometry. Our age estimates agree with abundance estimates from independent observations.     

基于上限分析的边坡稳定可靠性评估

从塑性极限分析出发,基于上限分析构建边坡极限状态可靠度计算模型;针对状态函数高度非线性导致常规可靠度方法求解时存在困难的问题,将响应面模型作为极限状态函数与可靠度计算间"桥梁",利用二次正交原理优化取样点,建立考虑参数相关性的二次响应面替代函数。利用JC法直接求得边坡可靠指标的一个上限解,讨论了单个及多个参数变异性对边坡可靠度的影响。     

Stability analysis of slopes reinforced with piles

In this paper, the kinematic approach of limit analysis is used to analyse the stability of earth slopes reinforced with piles. First, the case of slope without piles is considered and a procedure is developed to calculate the safety factor for the slope. Results are compared with those obtained using both the limit equilibrium method and more complex upper and lower bound limit analysis solutions. Then, the stability of slopes reinforced with piles is analysed. Expressions are derived allowing the force needed to increase the safety factor to a desired value and the most suitable location of piles within the slope to be evaluated. A study is carried out to illustrate the effect of piles on slope stability.     

顺层岩质边坡稳定性极限分析上限法

基于极限分析上限法理论,运用体积力增量法,考虑单层滑动面极限分析模型的缺陷,建立考虑含结构面的多岩层错动的任意块体模型,利用岩块体在外荷载作用下达到极限破坏时,外荷载做的功与岩体消耗的功相等为基础建立等式方程,由此推导得到此类边坡稳定系数的计算公式。在分析典型边坡算例的基础上,对比离散元数值模拟结果,验证了该方法的可行性和适用性。对云南省普宣高速公路某顺层岩质边坡进行计算,其稳定系数接近离散元数值模拟结果,数值稍有偏大,边坡稳定。其研究结果为此类边坡稳定性评价提供了一种新的计算方法。     

The upper geochronological limit for dunites of the East Khabarny gabbro-ultramafic complex (South Urals) by the data of U-Pb age of zircons extracted from vein hornblendites

This paper discusses the results of U-Pb isotopic dating of zircons from hornblendites that cut dunites of the East Khabarny dunite-clinopyroxenite-websterite-gabbro complex in the South Urals. This complex is included into the structure of the large Khabarny mafic-ultramafic allochthon, and the set of rocks and their petrogeochemical peculiarities allow this complex to be compared with the Ural-Alaskan-type complexes. Zircons from hornblendites have been dated on a SHRIMP-II ion microprobe and by the classical thermo-ionization mass spectrometric method by five fractions. The obtained results are comparable between each other within the analysis deviation interval and show that hornblendites were formed in the Early Devonian (408–402 Ma). This age is the upper geochronological limit in estimation of the time when dunites of the East Khabarny complex were formed. The synchronity of intrusive hornblendite manifestation in most of the Urals in the Early Devonian is discussed. The probable Early Devonian stage, in addition to the found Vendian and Ordovician-Silurian ones when dunite-clinopyroxenite-gabbro complexes formed in the Urals, is suggested.     

A calculation method for the embedded depth of stabilizing piles in reinforced slopes

Embedded stabilizing piles are a significant optimization measure for traditional piles used to reinforce slopes or landslides. The determination of the embedded depth of the pile top is essential for engineering design. On the basis of the potential overtop-sliding failure mechanism for a piled slope, the corresponding overall slip surface is assumed to consist of the upper part from the original slip surface of the landslide, and the lower part occurs in the local slide mass upslope of the piles. The imbalanced thrust force method is used to determine the thrust force of the upper slide mass, and a variational calculus method within the framework of limit equilibrium for the lower slide mass is provided to calculate its limit resistance. According to the equilibrium relationship between the thrust force and the limit resistance under a design factor of safety of the piled slope, a closed-form solution to the piled-slope stability is specifically derived. It can quantitatively exhibit the influences of some important factors, including the embedded depth on the factor of safety and the corresponding slip surface of the slope. The analysis results of some practical examples show that the factor of safety decreases nonlinearly as the embedded depth increases. The proposed method can be applied in practical engineering.     

雅砻江两河口水电站庆大河左岸边坡某变形体变形机制分析与稳定性预测

雅砻江两河口水电站泄洪建筑物进口布置于庆大河左岸边坡,继在边坡中下部圈定3个变形体后,在边坡上部发现变形体Ⅳ区,严重威胁泄洪建筑物的安全。通过探硐、赤平投影等手段,结合研究区地质环境,确定了边坡变形破坏机理,该边坡为中薄层岩体反倾边坡,青藏高原隆升伴随河流下切,边坡卸荷,在上部岩体自重作用下,坡脚薄层岩体发生倾倒弯折,河流侵蚀作用下变形加剧导致局部弯折贯通形成底滑面,在外力作用下崩滑破坏,上部变形体失去支撑后倾倒弯折破坏加剧,由于岩层薄,变形体多为碎裂散体结构。采用Geo-slope软件对变形体进行稳定性分析,结果表明自然状态下Ⅳ区变形体处于极限平衡状态,下部变形体清除后,Ⅳ区变形体失稳。最后,根据结果制定了合理的变形体处理措施。     

Studies of Star-forming Complexes in the Galaxies NGC 628, NGC 2976, and NGC 3351

The parameters of the radiation of interstellar matter in star-forming complexes in the high-metallicity galaxies NGC 628, NGC 2976, and NGC 3351, which have different morphological types, are analyzed. The relationship between the emission in Hα and in lines of CO and HI is considered, as well as the relationship between Hα and the emission of dust in the infrared range (IR). The fluxes and surface brightnesses in the UV and IR correlate well with the Hα emission. The HI emission also correlates well with Hα, while the correlation between the CO and Hα emission is much weaker. The ratio of the fluxes at 8 and 24 µm decreases with increasing Hα flux. This may be due to changes in the properties of the dust ensemble (a decrease in the mass fraction of polycyclic aromatic hydrocarbons) or to changing excitation conditions. Analysis of the kinematics of the CO lines shows that the CO flux grows with increasing velocity scatter ΔV when ΔV ? 70 km/s. Preliminary evidence for the existence of star-forming complexes with higher values of ΔV is provided, when the increase in the velocity scatter is accompanied by a decrease in the CO luminosity of the complex.

     

土体极限分析的基本方程与广义极限平衡法

对屈服条件与屈服函数的极值条件进行了讨论,在不需要流动法则的情况下建立了速度方程。平衡方程、屈服条件与屈服函数的极值条件、速度方程就是土体极限分析的基本方程。这样,对荷载、速度边界条件（包括荷载与速度边界同时存在）,均构成了完备的极限平衡问题。对边坡稳定问题的上、下限定理给出了严密的证明,并建立了求解极限平衡问题的广义极限平衡法,均质土的计算结果表明,圆弧滑动面的广义极限平衡法与对数螺旋面的上限解法基本一致。     

多阶多层复杂边坡稳定性的通用上限方法

极限分析上限方法在边坡稳定性评价中受到了广泛关注,但当前所取得的解析成果尚不能直接应用于解决任意多土层分布、多台阶的广义复杂层状边坡。基于组合对数螺线的旋转破坏机制,推导了具有任意坡面几何特征、任意多土层（含非水平土/岩层）边坡的外功率统一积分表达式及相应的虚功率方程,提出了多阶多层复杂边坡稳定性的通用极限分析上限方法;为克服积分式的复杂解析计算,引入了数值积分技术。在此基础上,结合最优化方法和强度折减技术,优化求解了复杂边坡的全局稳定性安全系数及相应的临界滑动面。通过多个典型算例的验证与对比分析,表明该方法具有较高的精度和广泛适用性。最后,针对典型多阶多层边坡实例,开展了上限法的深度拓展与应用研究,其结果为广义复杂层状边坡的稳定性评价提供了新思路。     

基于塑性极限分析上限法理论的土质边坡可靠度分析

将极限分析的上限定理、有限元离散思想、随机规划理论和蒙特卡洛方法这四者结合起来,提出了一种土质边坡可靠度分析的上限数值方法。首先采用三节点有限单元离散土质边坡,然后将土体的抗剪参数设为随机变量,根据上限定理构建同时满足三角形单元的塑性流动约束条件、单元公共边的塑性流动约束条件和单元速度边界条件的机动许可速度场,并根据内功功率等于外功功率条件建立目标函数,构建土质边坡可靠度分析的上限法随机规划模型。采用蒙特卡洛方法求解上限法随机规划模型,同时提出了一种基于上限法速度场的边坡失效风险系数估算方法,该方法特别适用于具有多种失效模式的边坡风险分析。对2个经典算例进行了深入分析,验证了方法的正确性。     

Parametric studies of disturbed rock slope stability based on finite element limit analysis methods

This study employs the finite element upper bound and lower bound limit analysis methods to investigate the stability of inhomogeneous rock slopes. The differences in the stability numbers of the upper and lower bound solutions are bracketed within ±10.5% or better, and the stability numbers obtained are presented in rock slope stability charts. These stability charts can provide a convenient tool for preliminary stability designs of inhomogeneous rock slopes. Various recommended blasting damage zones are considered, and disturbance factors are used to represent damage levels. Results showed that rock mass disturbance could significantly influence the evaluation of rock slope stability.     

膨胀变形对膨胀土边坡稳定性的影响

当采用合理的强度参数时,根据常规极限平衡或极限分析方法的计算结果,很难解释一些膨胀土边坡会在极缓的坡度下发生失稳破坏的原因。事实上,由于膨胀土遇水后会发生显著的变形,在饱和区与非饱和区交界面附近会出现很大的剪应力。因此,在膨胀土边坡的稳定分析中,需要考虑这种因素的影响。根据塑性力学的上限定理,严格地导出了考虑膨胀应力作功的功能平衡方程。根据强度储备定义的安全系数即隐含在这一方程中,它可以通过迭代方法求解。边坡稳定的上限分析在数值上是利用了单元集成法来完成的。这不仅能方便地利用应力分析的成果,而且能进行滑裂面的优化,从而找到最小的安全系数。对一个坡度为1:4的膨胀土边坡的稳定计算结果表明,膨胀变形会使边坡的安全系数显著减小。当考虑膨胀时,优化得到的破坏模式是在浅层出现一个局部的滑动,它会牵动其上部的土体也相继出现局部滑动,这正好符合膨胀土滑坡时所常见的牵引性的特征。