Distance to the Pulsar B1642–03 and the Influence of the H II Region S27 on Its Dispersion Measure and Scattering Parameters

Based on data on the dispersion measure and the interstellar-scattering parameters of the pulsar B1642–03, which is observed in the direction of the emission nebula S27 around the early-type star ζ Oph, it is concluded that this nebula makes a relatively small contribution to its dispersion measure (～9?23%) and scattering angle (～9?16%). It is shown that the distance to B1642–03 is 2.2–2.6 kpc.     

肇东和亳县陨石中的黑包体及其成因意义

肇东、毫县陨石中的黑包体在总体成分、形状、大小上与陨石球粒相似,但两者的内部结构以及矿物组合不同。黑包体中矿物呈密堆状,主要由细粒橄榄石以及其它硅酸盐微晶组成,不含火成玻璃等特点表明黑包体未经历过熔融,它们可能是形成球粒的毛坯。因此认为球粒的形成有三个阶段:星云凝聚形成尘粒—尘粒吸积形成黑包体—黑包体熔融形成球粒。     

Parameters for the dust envelope of the protoplanetary nebula IRAS 18062+2410

We have calculated a model for the dust envelope of the protoplanetary nebula IRAS 18062+2410 using observations from the ultraviolet to the far infrared. We assume that the envelope is spherically symmetrical and consists of identical silicate grains with a radius of 0.10 micron, and with the number density of the grains inversely proportional to the square of the distance. The optical depth of the envelope, whose inner boundary is 1.40×10^?3 pc from the center of the star, is 0.050 at 10 microns. At the inner envelope boundary, the temperature of the dust grains is 410 K and their density is 2.7×10^?7 cm^?3. Using calculations of stellar evolution at the stage following the exit from the asymptotic giant branch, we estimate the dust envelope’s expansion velocity to be 12 km/s. The mass-loss rate of the star preceding the ejection of the envelope was about 4.5×10^?6 M _⊙/yr. The observed excess of far-IR flux is not associated with the continuum radiation of the nebula, and may provide evidence for the presence of dust ejected by the star in earlier stages of its evolution.     

Dust in galaxy clusters

The conditions for the destruction of dust in hot gas in galaxy clusters are investigated. It is argued that extinction measurements can be subject to selection effects, hindering their use in obtaining trustworthy estimates of dust masses in clusters. It is shown, in particular, that the ratio of the dust mass to the extinction M _d /S _d increases as dust grains are disrupted, due to the rapid destruction of small grains. Over long times, this ratio can asymptotically reach values a factor of three higher than the mean value in the interstellar medium in the Galaxy. This lowers dust-mass estimates based on measurements of extinction in galaxy clusters. The characteristic lifetime of dust in hot cluster gas is determined by its possible thermal isolation by the denser medium of gas fragments within which the dust is ejected from galaxies, and can reach 100–300 million years, depending on the kinematics and morphology of the fragments. As a result, the mass fraction of dust in hot cluster gas can reach 1–3% of the Galactic value. Over its lifetime, dust can also be manifest through its far-infrared emission. The emission characteristics of the dust change as it is disrupted, and the ratio of the fluxes at 350 and 850 μm can increase appreciably. This can potentially serve as an indicator of the state of the dust and ambient gas.     

A model for the dust envelope of the protoplanetary nebula LSIV-12°111

A model for the dust envelope of the protoplanetary nebula LSIV-12°111 is computed using measured fluxes of the object from the UV to the far-IR. It is assumed that the spherically symmetrical envelope is comprised of silicate particles with a standard MRN size distribution, whose number density varies inversely proportional to the square of the distance. The optical depth of the envelope, whose inner boundary is 5.6×10¹⁶ cm from the central star, is 0.072 at 0.55 µm. The temperature of the dust grains at the inner boundary of the envelope is 124 K. The estimated distance to LSIV-12°111 is 3.8 kpc. The current mass-loss rate of the object derived from a self-consistent solution for the radiative transport and motion of the dust in the envelope is 1.0×10^?5M_⊙/yr.     

内蒙古中西部地区土壤水分对沙尘暴的贡献

以2001年4月至2002年 6月内蒙中部地区逐时观测的土壤水分资料为基础，论证了该区日土壤水分和日平均风速的变化规律，统计分析了日平均风速与土壤水分对沙尘暴的成生综合贡献。得出的主要结论是：①该地区沙尘暴发生时日平均风速的最小值是 3．5 m／s。如果日平均风速大于 8．0 m／s，预示着有沙尘暴的发生。②在平均风速大于 3．5 m／s的条件下，观测样本中 18．4％日数发生沙尘暴，而81．6％日数没有发生。说明大风的天气条件不应当被视其为沙尘暴的唯一重要的因子。③在同一地点、同样的风力条件下，在沙尘暴发生时，日平均风速与日平均土壤水分呈明显的反相关变化；而它们的反相关关系不明显时，沙尘暴就很少发生。     

内蒙古中西部地区土壤水分对沙尘暴的贡献

以2001年4月至2002年6月内蒙中部地区逐时观测的土壤水分资料为基础，论证了该区日土壤水分和日平均风速的变化规律，统计分析了日平均风速与土壤水分对沙尘暴的成生综合贡献。得出的主要结论是：①该地区沙尘暴发生时日平均风速的最小值是3．5m／s。如果日平均风速大于8．0m／s，预示着有沙尘暴的发生。②在平均风速大于3.5m／s的条件下，观测样本中18．4％日数发生沙尘暴，而81．6％日数没有发生。说明大风的天气条件不应当被视其为沙尘暴的唯一重要的因子。③在同一地点、同样的风力条件下，在沙尘暴发生时，日平均风速与日平均土壤水分呈明显的反相关变化；而它们的反相关关系不明显时，沙尘暴就很少发生。     

Infrared emission and the destruction of dust in HII regions

The generation of infrared (IR) radiation and the observed IR-intensity distribution at wavelengths of 8, 24, and 100 µm in the ionized hydrogen region around a young, massive star is investigated. The evolution of the HII region is treated using a self-consistent chemical-dynamical model in which three dust populations are included—large silicate grains, small graphite grains, and polycyclic, aromatic hydrocarbons (PAHs). A radiative transfer model taking into account stochastic heating of small grains and macromolecules is used to model the IR spectral energy distribution. The computational results are compared with Spitzer and Herschel observations of the RCW 120 nebula. The contributions of collisions with gas particles and the radiation field of the star to stochastic heating of small grains are investigated. It is shown that a model with a homogeneous PAH content cannot reproduce the ring-like IR-intensity distribution at 8 µm. A model in which PAHs are destroyed by ultraviolet radiation of the star, generating region HII, provides a means to explain this intensity distribution. This model is in agreement with observations for realistic characteristic destruction times for the PAHs.     

沙尘天气过程临界起沙因子的研究进展

临界起沙摩阻风速u*t或临界起沙风速ut是土壤可蚀性的度量指标之一,是表征沙尘颗粒进入大气的重要因子,也是沙尘暴预报模块中最重要的参数之一.野外实验、模式参数化和统计理论是近年来确定临界起沙摩阻风速u*t或临界起沙风速ut的3种主要方法.利用不同方法获取u*t或ut的结果可以相互校验.野外实验的实测结果可为获取适用的起...     

Vortex motions and transportation of fine disperse dust particles in the ionosphere

Redistribution of dust particles in the ionosphere as a result of vortical motions is discussed. The following possibilities are studied: capture and evolution of dust particles in acoustic-gravitational (AG) vortices, formation of dust vortices as a result of involving a great number of dust particles into vortex motions, and formation of vertical dust flows (streamers). It is shown that excitation of AG-vortices at altitudes of 110–130 km as a result of development of AG-wave instability, associated with non-zero balance of heat fluxes, owing to solar radiation, water vapors condensation, infrared emission of the atmosphere, and thermal conductivity, leads to a substantial transportation of dust particles and their mixing at altitudes of 110–120 km. Layers of dust particles in the ionosphere with a thickness of about a kilometer, forming at altitudes less than 120 km, distribute within the region of existence of AG-vortical structures. As a result, at altitudes of 110–120 km, dust vortices can appear, and transportation of particles up to altitudes of 130 km becomes possible. One of the ways of transportation of dust particles in the ionosphere is vertical flows (streamers), which are generated by dust vortices as a result of development of parametric instability.     

亚洲沙尘的远距离输送及对海洋生态系统的影响

亚洲沙尘是全球沙尘的重要组成部分,其环境效应已得到广泛关注,但至今对亚洲沙尘输送/沉降—海洋生态系统响应—辐射活性气体海气交换—间接气候效应这一过程的认识却是非常初步的。亚洲沙尘存在3个主要源区,对其排放强度的认识仍存在较大的不确定性。亚洲沙尘可以通过长距离输送而影响到广大的北太平洋,其传输路径和影响范围决定于沙尘的来源、粒子谱分布与大气环流特征等因素。沙尘沉降是海洋营养物质和污染物质的来源之一,但沉降通量的估算结果仍有待进一步验证,而对海洋生态系统的作用机制及其反馈还缺乏足够的了解。论文在综述国内外相关研究的基础上,提出了“亚洲沙尘与海洋生态系统”（Asian Dust and Ocean EcoSystem,ADOES）研究计划的科学目标和主要研究内容。     

粉尘释放和沉积机制的研究进展

风蚀地表释放的粉尘气溶胶在其输送和沉积过程中产生的直接和间接环境效应促进了对其释放和沉积机制的研究.随着土壤风蚀研究的发展,对粉尘释放机制有了较为深入地研究,从简单的经验方程模型发展到目前考虑粉尘释放微观过程的具有清晰物理机制的释放模型,并在大尺度沙尘预报研究中得到了广泛应用.粉尘沉积主要集中于对干沉积和云下清除过程的研究,而对云内清除过程认识不足.简要回顾了粉尘释放和沉积机制研究的发展历史,系统地评述了研究的现状,提出了粉尘释放和沉积模拟研究中存在的问题和今后的发展趋势.     

The origin of organic matter in the solar system: evidence from the interplanetary dust particles

The detailed examination of meteorites and interplanetary dust particles provides an opportunity to infer the origin of the organic matter found in primitive Solar System materials. If this organic matter were produced by aqueous alteration of elemental (graphitic or amorphous) carbon on an asteroid, then we would expect to see the organic matter occurring preferentially in interplanetary materials that exhibit evidence of aqueous activity, such as the presence of hydrated silicates. On the other hand, if the organic matter were produced either during the nebula phase of Solar System evolution or in the interstellar medium, we might expect this organic matter to be incorporated into the dust as it formed. In that case pre-biotic organic matter would be present in both the anhydrous and the hydrated interplanetary materials. We have performed carbon X-ray absorption near-edge structure spectroscopy and infrared spectroscopy on primitive anhydrous and hydrated interplanetary dust particles (IDPs) collected by NASA from the Earth's stratosphere. We find that organic matter is present in similar types and abundances in both the anhydrous and the hydrated IDPs, and, in the anhydrous IDPs some of this organic matter is the “glue” that holds grains together. These measurements provide the first direct, experimental evidence from the comparison of extraterrestrial samples that the bulk of the pre-biotic organic matter occurs in similar types and abundances in both hydrated and anhydrous samples. This indicates that the bulk of the pre-biotic organic matter in the Solar System did not form by aqueous processing, but, instead, had already formed at the time that primitive, anhydrous dust was being assembled. Thus, the bulk of the pre-biotic organic matter in the Solar System was formed by non-aqueous processing, occurring in either the Solar nebula or in an interstellar environment. Aqueous processing on asteroids may have altered this pre-existing organic matter, but such processing did not affect in any substantial way the C=O content of the organic matter, the aliphatic C-H abundance, or the mean aliphatic chain length.     

Polycyclic aromatic hydrocarbons in the dwarf galaxy IC 10

Archival infrared Spitzer Space Telescope observations are used to study the dust component of the ISM in the irregular galaxy IC 10. The dust distribution in the galaxy is compared to the distributions of the Hα and [S II] emission, neutral gas and CO clouds, and ionizing radiation sources. The distribution of polycyclic aromatic hydrocarbons (PAHs) in the galaxy is shown to be highly non-uniform, with the fraction of these particles in total dust mass reaching 4%. On the whole, PAHs avoid bright H II regions and correlate with the atomic and molecular gas. This pattern suggests that they form in the dense interstellar gas. It is suggested that the observed metallicity dependence of the PAH abundance shows up not only globally (at the level of the entire galaxy), but also locally (at least, at the level of individual H II regions). No conclusive evidence for shock destruction of PAHs in the IC 10 galaxy has been found.     

Mathematical simulation of complex natural systems

The paper presents a review of publications devoted to the mathematical simulations of natural systems whose large spatiotemporal scales make impossible their adequate experimental modeling in nature. The studies include the modeling of the mineralogy of the surface rocks of Venus and Mars, fractional condensation from the gaseous constituent of the preplanetary nebula, the genesis of chondrites and the material of the Earth’s upper mantle, and the evaporation of interstellar dust and the stratification of material in cooling planets.     

应用同步辐射微束X射线荧光光谱法研究单个大气PM2．5颗粒物的源特征

将高灵敏度的同步辐射微束x射线荧光光谱分析方法与计算机模式识别技术相结合，用于上海市大气PM2.5，单颗粒物的源识别。分析了污染排放源的PM2.5，单颗粒物，结果表明，来自不同污染排放源的颗粒物具有不同的能谱特征。同时分析了环境空气监测样品PM2.5，单颗粒物，结果表明，在上海市中心区大气PM2.5，的污染源主要以机动车尾气为主，而在吴淞工业区大气PM2.5，的污染源主要以钢铁工业尘和燃煤烟尘为主。     

Polarimetry of the protoplanetary nebula AFGL 2688

Our spectroscopic (with resolution R=75 000) and spectropolarimetric (R=15 000) observations with the 6-m telescope of the Special Astrophysical Observatory have enabled us to distinguish photospheric and circumstellar features in the optical spectrum of the bipolar protoplanetary nebula AFGL 2688 for the first time. The linear polarization of the radiation was measured at 5000–6600 Å. The emission in the lines of the sodium doublet and the Swan bands is formed in the envelope, and the mechanism exciting the transitions is resonance fluorescence. We conclude that the circumstellar envelope has a low density. Features of the structure of the nebula are discussed based on published high-angular-resolution photometric and polarimetric (HST NICMOS) data.     

Progress on Process and Mechanism of Sand and Dust Emission on Gobi

Gobi is one of the most important landscapes in northwest China, and it is also one of the dust sources in north China and even in central Asia. Based on the different land surface characteristics on the gobi surface, sand and dust emission process and mechanism are obviously different with other landscapes, such as sandy desert. Dust emission process and mechanism on the gobi surface were analyzed in this paper. Wind power system, geomorphology pattern and underlying characteristics were considered for their effect on the sand and dust emission process. Then, the mechanism of land surface characteristics on threshold wind velocity was analyzed. Finally, based on the previous studies on dust emission and mechanism, and in combination with the regional and global requirement, we suggested that the land surface characteristics parameterization, identification of the dust sources and sediment emission mechanism should be the main issues in the future gobi sand and dust research.     

Macromolecules in the galaxy and the cosmic microwave background

A deep search for the predicted Galactic microwave dipole emission of spinning interstellar fullerene-type molecules has been conducted using the RATAN-600 radio telescope. This effect is of interest both in its own right and as a new form of Galactic screen between the cosmic microwave background (CMB) and the observer. The power of this noise component on angular scales of about 0.1° (l=1000) is estimated. These scales are of primary interest for the “Cosmological Gene of the Universe” (RATAN-600), PLANCK Surveyor Mission, and other projects. At the frequencies of the expected emission peak of this dust component, the small-scale noise is a factor of 20 weaker than the predicted noise. It is shown that the role of this dust component is negligible, at least at the main PLANCK frequencies. The first estimates of the contribution from Galactic polarization noise are given for λ=3.9 cm, where the theory predicts a maximum in the CMB polarization (l～1000). At wavelengths of ～1 cm and shorter, macromolecules contribute less than 1 µK, and should not hinder CMB polarization studies. Galactic synchrotron polarization, likewise, should not prevent CMB polarization experiments at the main PLANCK frequencies.     

Surface properties of the Orgueil meteorite: implications for the early history of solar system volatiles

Dehydration of Orgueil by stepwise calcination produced more than a tenfold change in its Kr B.E.T. surface area, which increased to 120 m²/g, then fell to 40 m²/g. This phenomenon characterizes structures of the montmorillonite type, but not other plausible constituents of Orgueil. It results from vacating of interlayer sites by H₂O molecules which are replaced by Kr until finally the sheets collapse, excluding Kr. Differential calorimetric scans of Orgueil also gave a better match for montmorillonite than for other minerals. However, a simple identification as montmorillonite conflicts with chemical analyses of Orgueil phyllosilicates.Exchangeability of H₂O in Orgueil was shown by water regain from lab air between calcination cycles and similarily of the cycles. Room temperature dehydration revealed up to 6 per cent free surface adsorbed water. High D/H ratios in CI's may result from D enrichment in OH^? groups during equilibration of dispersed phyllosilicate dust with nebula gas at temperatures ?0°C. Adsorption on the very large free and interlayer surface areas of this dust was the major mechanism by which volatiles still uncondensed at the time of gas-dust separation (including planetary primordial Ar, Kr and Xe) were incorporated into solid solar system material.