Self-similar regimes for the collapse of magnetic protostellar clouds

Self-similar solutions describing the homogeneous, free, isothermal collapse of protostellar clouds are considered. One such solution correponds to the critical case of the propagation of a rarefaction wave near the time when it is focused in the central region of the cloud. The speed of the rarefaction front is finite and equal to three times the isothermal sound speed. The asymptotic distributions of gas-dynamical quantities in the central part of the collapsing cloud and the surrounding envelopes are considered at both early and late stages of compression, after the formation of an opaque core (protostar). These solutions are used in a magneto-kinematic approximation to study the geometry and evolution of the large-scale magnetic fields of collapsing protostellar clouds. All the solutions are verified using direct numerical simulations. It is shown that an initially uniform magnetic field acquires an “hourglass” geometry with time. The characteristic opening angles in the self-similar solutions are in satisfactory agreement with observations.     

Determining the parameters of massive protostellar clouds via radiative transfer modeling

A one-dimensional method for reconstructing the structure of prestellar and protostellar clouds is presented. The method is based on radiative-transfer computations and a comparison of theoretical and observed intensity distributions at both millimeter and infrared wavelengths. The radiative transfer of dust emission is modeled for specified parameters of the density distribution, central star, and external background, and the theoretical distribution of the dust temperature inside the cloud is determined. The intensity distributions at millimeter and IR wavelengths are computed and quantitatively compared with observational data. The best-fit model parameters are determined using a genetic minimization algorithm, which makes it possible to reveal the ranges of parameter degeneracy as well. The method is illustrated by modeling the structure of two infrared dark clouds IRDC-320.27+029 (P2) and IRDC-321.73+005 (P2). The derived density and temperature distributions can be used to model the chemical structure and spectral maps in molecular lines.     

A multicomponent model for computing the thermal structure of collapsing protostellar clouds

A model for simulating the thermal and dynamical evolution of protostellar clouds is presented. In the model, the dust and gas temperatures are treated separately, making it possible to more precisely describe the initial stages of the cloud’s gravitational contraction and collapse. The model is fast enough to be applied in hydrodynamical computations, and has a high enough accuracy for the results to be used to compute emission spectra and comparing them with observational data. Two problems are considered as test examples and simple applications: calculation of the structure of clouds in thermal and hydrostatic equilibrium, and modeling the evolution of a protostellar cloud in a spherically symmetric approximation, including the formation of the first hydrostatic core.     

Modeling of the formation of complex molecules in protostellar objects

The results of molecular composition modeling are presented for the well studied low-mass star-forming region TMC-1 and the massive star-forming region DR21(OH), which is poorly studied from a chemical point of view. The column densities of dozens of molecules, ranging from simple diatomic to complex organic molecules, are reproduced to within an order of magnitude using a one-dimensional model for the physical and chemical structure of these regions. The chemical ages of the regions are approximately 105 years in both cases. The main desorption mechanisms that are usually included in chemical models (photodesorption, thermal desorption, and cosmic-ray-induced desorption) do not provide sufficient gasphase abundances of molecules that are synthesized in surface reactions; however, this shortcoming can be removed by introducing small amount of reactive desorption into the model. It is possible to reproduce the properties of the TMC-1 chemical composition in a standard model, without requiring additional assumptions about an anomalous C/O ratio or the recent accretion of matter enriched with atomic carbon, as has been proposed by some researchers.     

Influence of luminosity bursts on properties of protostellar disks

A (2+ 1)-dimensional numerical model for the formation and evolution of young stellar objects with sub-solar masses is presented. The numerical hydrodynamicall code describing the formation and evolution of a pølar disk in a two-dimensional approximation is supplemented by one-dimensional code for the evolution of the star and an algorithm for establishing the vertical structure of the disk. This code is used to investigate the influence of luminosity bursts with intensities similar to those observed in FU Orionis objects (FUors) on the properties and thermal balance of pølar disks. A model with gravitational instability and fragmentation of the disk, with subsequent migration of the fragments onto the protostar, is used as a basic model for FUors. Typical FUor bursts (L ～ 100 L ^⊙) can appreciably influence the thermal balance of their disks and parent envelopes, leading to an increase in the disk temperature by more than a factor of two. On the other hand, massive fragments in the disk are only weakly perturbed by such bursts, partially due to screening by the disk and partially due to their high temperature brought about by adiabatic heating. Apart from massive fragments, the characteristic thermal time scales are appreciably shorter than the dynamical time scales throughout the radial extent of the disk and envelope; this enables the use of a stationary radiative-transfer equation when determining the vertical structure of the disk.     

Different-sized dust grains and the chemical evolution of protostellar objects

Results of modeling the chemical evolution of protostellar objects are presented. The models take into account the existence of different dust populations with distinct grain sizes, total mass fractions, and temperatures. In addition to ”classical” dust grains, the models include an entirely different second dust population, with dust grain sizes of 30 Å and a higher temperature. Two chemical-evolution models are compared, one taking into account only classical dust and the other including both dust populations. The influence of a complex dust composition on the general evolution of the molecular contents of prestellar cores and the abundances of a number of chemical species is studied. At early evolutionary stages, differences are mainly determined by the modification changes in the photoprocesses’ balance due to efficient UV absorption by the second population of dust grains and in collisional reactions with the dust grains. At late stages, distinctions between the models are also determined by the increasing dominance of additional reaction channels. The species that respond to the presence of small grains in different ways are separated into different groups. Allowing for the presence of small grains makes it possible to significantly lower the water abundance in the gas phase.     

Physical properties of molecular clouds as functions of their Galactocentric distance from CS and C<Superscript>34</Superscript>S observations

Twenty-eight CS molecular clouds toward HII regions with Galactocentric distances from ～ 4 to 20 kpc have been studied based on observations obtained in the J=2→1 lines of CS and C³⁴S on the 20-meter radio telescope of the Onsala Space Observatory (Sweden) in March 2001. All 28 clouds have been mapped with an angular resolution of ～40″. The peak intensity in the C³⁴S line has been measured for 20 objects. An LTE analysis has been performed and the parameters of the molecular cloud cores derived. The core sizes are d_A=0.3–4.8 pc, with a median value of ～1.6 pc. The mean hydrogen densities in the cloud cores are n_H2=3.5×10²–3.7 × 10⁴ cm^?3, with a median value of ～7.2×10³ cm^?3. The value of n_H2 ends to decrease with increasing Galactocentric distance of the cloud. The masses of most clouds are 10²?6×10³M_⊙, with the most probable value being M_CS～10³M_⊙. The data follow the dependence M_CS ∝d _A ^(2.4–3.2) . As a rule, the cloud masses are lower than the virial masses for M_CS<10³M_⊙.     

Variations in the accretion rate and luminosity in gravitationally unstable protostellar disks

Self-consistent modeling of a protostar and protostellar disk is carried out for early stages of their evolution. The accretion rate at distances of sevral astronomical units from the protostar is appreciably variable, which is reflected in the protostar’s luminosity. The amplitude of the variations in the accretion rate and luminosity grows together with the sampling period, as a consequence of the nature of gravitationally unstable protostellar disks. A comparison of model luminosity variations with those derived from observations of nearby sites of star formation shows that the model variations are appreciably lower than the observed values for sampling periods of less than 10 years, indicating the presence of additional sources of variability on small dynamical distances from the protostar.     

常用小波及其时频特性

小波分析以其良好的时频局部化效果,能够用来分析时间序列不同频率的非稳定能量特征。目前,有许多可供选择的小波函数,这些函数的时频特征各不相同,根据研究目的选择合适的分析小波函数就显得非常重要。针对常用的几个实数和复数小波函数,以Nino3海面季度平均温度时间序列(1871-1996,5oS~5oN, 90o~150oW)为例,分别研究它们的时频特征,希望为实际应用过程中选择合适的分析小波提供依据。研究发现,消失矩越大,时域小波越窄,时间分辨率增强,波动幅度越大;而频域小波与时域相反。复数的Morlet小波具有良好的频率分析能力,而Mexican hat小波(Gauss函数的二阶导数)则具有优秀的时间分辨能力。相对小波的总能量谱,复数小波的实部或虚部的能量谱能够明显提高分析结果的时间分辨率,但并不影响小波的频域分辨力。     

High-pressing preparation of rock glasses and their elastic properties

Melt glasses for seven types of rock ranging from acid to basic were prepared under 1.0 GPa on a multi-anvil pressure apparatus, YJ-3000 ton press. Densities and elastic properties of the melt glasses were compared with those described in previous studies. It was found that the glasses melted under 1.0 GPa were consistent in density with both naturally-occurring glassy rocks and artificially prepared glasses melted at ambient pressure. The densities of glasses are negatively correlated with the SiO2 contents and positively correlated with the （MgO＋FeO） contents. The compressive velocity （Vp） of glass tends to increase with decreasing SiO2 contents and increasing （MgO＋FeO） contents. The shear velocity （Vs） of glass tends to increase slightly with increasing SiO2 contents, which has little connection with the （MgO＋FeO） contents. It was calculated from densities and velocities that the elastic moduli of glasses are negatively correlated with the SiO2 contents and positively correlated with the （MgO＋FeO） contents.     

Some thermodynamical and microphysical aspects of monsoon clouds

The thermodynamical and microphysical characteristics of monsoon clouds in the Poona, Bombay and Rihand regions were investigated using extensive aircraft in-cloud observations. The number of clouds sampled at Poona, Bombay and Rihand is 2199, 169 and 104 respectively. The temperatures inside the cloud are colder than its environment at Poona and Rihand. The maximum difference is about 3°C at the cloud base level and the difference decreased with height. At Bombay the difference is less than 1°C and at some levels the temperatures inside the cloud are warmer than its environment. The lapse rates of temperatures inside the cloud are slightly less than those in the immediate environment of the cloud. The environmental lapse rates are nearly equal to the saturated adiabatic value. The positive increments in liquid water content (LWC) are associated with the increments in temperature inside the cloud. Similarly positive increments in temperatures inside the cloud are associated with the increments in temperature of its immediate environment at the same level or the layer immediately above. The maximum cloud lengths observed at Poona and Bombay respectively are 14 and 3 km. The horizontal cross-section of LWC showed a maximum number of 13 peaks in clouds at Poona while only 7 peaks were observed at Bombay. The location of maximum LWC in the horizontal cross-section is more or less at the centre of the cloud. The LWC profile showed an increase with height from the base of the cloud at Poona and Bombay. There is no marked variation of LWC with height at Rihand. The total droplet concentration at different altitudes at Poona and Bombay is in the range 28–82 cm^?3. The size distribution of cloud droplets experienced a broadening effect with increase in height from the cloud base at Poona. The broadening effect at Bombay is not as marked as that at Poona.     

The origin of giant molecular clouds

The parameters of molecular clouds formed via the Parker instability with dominant radiative losses are estimated. In this scenario, the cloud parameters (such as their mean densities and masses) should depend on galactocentric radius. This dependence is determined mainly by radial variations of the gas metallicity and the flux of heating radiation in the Galaxy. Due to the development of the interchange mode of the Parker instability, the angular momentum of the clouds will not necessarily be parallel to the galactic rotation axis.     

岩石裂隙的非饱和渗透特性及其演化规律研究

岩石裂隙的非饱和渗透特性是岩土、能源和环境等领域科学研究中的热点问题。采用三维激光扫描获取花岗岩裂隙的表面形貌特征,分析裂隙微观形貌特征对非饱和渗透特性的影响。研究在张拉、压缩、剪切等复杂荷载作用下裂隙开度分布的演化规律,建立复杂荷载作用下岩石裂隙非饱和毛细压力曲线演化模型。基于裂隙的微观形貌特征推导了岩石裂隙非饱和相对渗透系数模型,通过与试验数据对比,验证了模型的准确性和有效性,并在此基础上建立了复杂荷载作用下岩石裂隙非饱和相对渗透系数演化模型。研究成果对非饱和条件下裂隙岩体的水-力耦合机制研究具有一定指导意义。     

Geotechnical properties of Kuwaiti “gatch” and their improvement

Due to the difficulties experienced with the so-called gatch soils, the Ministry of Public Works of Kuwait engaged the services of the firm DORSCH, Consulting Engineers of Munich, Germany, to study the properties of gatch and to recommend methods to improve its suitability for road construction. An investigation program was agreed upon and selected samples were obtained from Kuwait.Prior to the geotechnical tests, mineralogical analyses were carried out. Surprisingly they found no trace in the samples of gypsum which was believed to cause damage to the highways built on gatch. The geotechnical tests performed indicated that the gatch soils were very sensitive to moisture and were therefore unsuitable as highway construction materials. However, their properties could be improved by various stabilization methods. It was found that cement stabilization was the most promising method since it not only increased the bearing capacity of the soil but also reduced its swelling characteristics.     

普通球粒陨石的物理和岩石学性质及其分类参数

不同球粒陨石群的物理和岩石学性质,包括球粒的平均大小、球粒结构类型、复合球粒、带火成边球粒及含硫化物的比例、化学组成及矿物学特征等可用以划分球粒陨石的化学-岩石类型和小行星类型,这些性质提供了不同球粒陨石群有用的分类参数及其形成环境的信息.由于不同球粒陨石群的△17O与日心距离存在有相关关系,因此,依据不同球粒陨石群形...     

Modeling of elastic and electrical properties of solid-liquid rock system with fractal microstructure

In the present paper we study the possibility of using joint quantitative interpretation of experimental electromagnetic and seismic data for lithospheric studies and to establish the situations in which the joint inversion of seismic and EM experimental data is possible. For this purpose a theoretical model of a solid-liquid rock mixture with fractal structure of grain-to-grain contact (Bahr, 1997; Spangenberg, 1998) was used to investigate dependence of elastic and electrical properties on rock microstructure. The electrical conductivity and seismic wave velocity were estimated by Monte-Carlo modeling for low porosity water-saturated crystalline rock and olivine-partially molten basalt system. It was shown that both elastic properties and conductivity of solid-liquid rock mixture depend non-linearly upon two main common factors, i.e. amount of liquid phase and fractal rock microstructure that is controlled by the degree of contact between grains. The dependence of rock physical macroproperties (seismic velocities, electrical conductivity and seismic and electrical anisotropy) upon these two main factors makes it possible to construct algorithms for joint quantitative interpretation of experimental seismic and electromagnetic data.     

Formation of organic substances of humus nature and their biospheric properties

Hypotheses of humus formation on the basis of polymerization and oxidation reactions were considered. The most popular models of several authors and the general understanding of the structural features of natural polymers were analyzed. Multivariate statistical analysis was performed for zonal factors affecting the formation of humic substances. Evolutionary changes in the understanding of the biospheric functions of humus substances were evaluated. Statistical procedures were proposed for the prediction of the physicochemical behavior of humus substances in environments.     

Dielectric Properties of Minerals and Their Applications in Microwave Remote Sensing

With the advantages of all-weather operation and certain penetration microwave remote sensing has become a very important technique,Its image is a function not only of the technical parameters of the sensor but also of the geometric forms and electrical properties,such as the dielectric constants and conductivity,of the ob jects on the ground.Minerals and rocks are the most widspread objects on the earth surface,hence their dielectric properties are of fundamental significance in microwave remote sensing.