Large scale structure of the universe

The current situation with the cosmological model and fundamental constants is briefly reviewed. Here, we concentrate on evolutionary effects of large-scale structure formation, in particular, the relationship with the quasar distribution and dynamics is discussed. We argue that groups of bright quasars with few or more than dozen of members within regions l _LS(100–150)h ^–1 Mpc found atz<2 may belong to concentrations of young rich clusters of galaxies, and thus be distant Great Attractors like the local GA or the Shapley concentration. These early large-scale galactic structures (i) provide a natural way to bias the distribution of Abell clusters, and (ii) suggest that the spectrum of primordial density perturbations is nearly flat on scales encompassing both the cluster and GAs,l=k ^–1(10,100)h ^–1 Mpc: _k ² k ³ P(k) k , =1 _–0.4 ^+0.6 , whereP(k) is the power spectrum of density perturbations.     

GEMS at the Galactic Cosmic-Ray Source

Galactic cosmic rays probably predominantly originate from shock-accelerated gas and dust in superbubbles. It is usually assumed that the shock-accelerated dust is quickly destroyed by sputtering. However, it may be that some of the dust can survive bombardment by the high-metallicity gas in the superbubble interior, and that some of that dust has been incorporated into solar system materials. Interplanetary dust particles (IDPs) contain enigmatic submicron components called GEMS (Glass with Embedded Metal and Sulfides). These GEMS have properties that closely match those expected of a population of surviving shock-accelerated dust at the GCR source (Westphal and Bradley in Astrophys. J. 617:1131, 2004). In order to test the hypothesis that GEMS are synthesized from shock-accelerated dust in superbubbles, we plan to measure the relative abundances of Fe, Zr, and Mo isotopes in GEMS using the new Resonance Ionization Mass Spectrometer at Argonne National Laboratory. If GEMS are synthesized from shock-accelerated dust in superbubbles, they should exhibit isotopic anomalies in Fe, Zr and Mo: specificially, enhancements in the r-only isotopes ⁹⁶Zr and ¹⁰⁰Mo, and separately in ⁵⁸Fe, should be observed. We review also recent developments in observations of GEMS, laboratory synthesis of GEMS-like materials, and implications of observations of GEMS-like materials in Stardust samples.     

Understanding Galaxy Formation with ISO Deep Surveys

We present the results obtained through the various ISO extragalactic deep surveys. Although IRAS revealed the existence of galaxies forming stars at a rate of a few tens (LIRGs) or even hundreds (ULIRGs) solar masses in the local universe, ISO not only discovered that these galaxies were already in place at redshift one, but also that they are not the extreme objects that we once believed them to be. Instead they appear to play a dominant role in shaping present-day galaxies as reflected by their role in the cosmic history of star formation and in producing the cosmic infrared background detected by the COBE satellite in the far infrared to sub-millimeter range. Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands, and the United Kingdom), and with the participation of ISAS and NASA.     

The Formation Of The First Stars In The Universe

In this review, I survey our current understanding of how the very first stars in the universe formed, with a focus on three main areas of interest: the formation of the first protogalaxies and the cooling of gas within them, the nature and extent of fragmentation within the cool gas, and the physics – in particular the interplay between protostellar accretion and protostellar feedback – that serves to determine the final stellar mass. In each of these areas, I have attempted to show how our thinking has developed over recent years, aided in large part by the increasing ease with which we can now perform detailed numerical simulations of primordial star formation. I have also tried to indicate the areas where our understanding remains incomplete, and to identify some of the most important unsolved problems.     

The James Webb Space Telescope

The James Webb Space Telescope (JWST) is a large (6.6 m), cold (<50 K), infrared (IR)-optimized space observatory that will be launched early in the next decade into orbit around the second Earth–Sun Lagrange point. The observatory will have four instruments: a near-IR camera, a near-IR multiobject spectrograph, and a tunable filter imager will cover the wavelength range, 0.6 < ; < 5.0 μ m, while the mid-IR instrument will do both imaging and spectroscopy from 5.0 < ; < 29 μ m.The JWST science goals are divided into four themes. The key objective of The End of the Dark Ages: First Light and Reionization theme is to identify the first luminous sources to form and to determine the ionization history of the early universe. The key objective of The Assembly of Galaxies theme is to determine how galaxies and the dark matter, gas, stars, metals, morphological structures, and active nuclei within them evolved from the epoch of reionization to the present day. The key objective of The Birth of Stars and Protoplanetary Systems theme is to unravel the birth and early evolution of stars, from infall on to dust-enshrouded protostars to the genesis of planetary systems. The key objective of the Planetary Systems and the Origins of Life theme is to determine the physical and chemical properties of planetary systems including our own, and investigate the potential for the origins of life in those systems. Within these themes and objectives, we have derived representative astronomical observations.To enable these observations, JWST consists of a telescope, an instrument package, a spacecraft, and a sunshield. The telescope consists of 18 beryllium segments, some of which are deployed. The segments will be brought into optical alignment on-orbit through a process of periodic wavefront sensing and control. The instrument package contains the four science instruments and a fine guidance sensor. The spacecraft provides pointing, orbit maintenance, and communications. The sunshield provides passive thermal control. The JWST operations plan is based on that used for previous space observatories, and the majority of JWST observing time will be allocated to the international astronomical community through annual peer-reviewed proposal opportunities.     

防风网对煤堆遮风效果的风洞实验研究

为了考察防风网对堆场煤堆的遮风效果,进行了防风网与煤堆之间区域的流场可视化实验。使用风洞模拟大气边界层条件,并将开孔率为38．5％的防风网模型布置在煤堆模型前方。实验中采用粒子成像测速（PIV）系统测量了防风网和堆场区域的平均风速分布,并且获得了煤堆表面的摩擦风速分布,进一步估算煤堆起尘量的变化情况。实验发现,防风网可有效降低煤堆表面迎风区域的摩擦风速,而对背风面的流场分布影响较小。研究结果可为防风网的遮护作用提供一定的实验支持。     

航空燃气涡轮发动机燃烧室的NOx控制及预测

:概述了燃气涡轮发动机中NOx的生成机理以及影响因素,简要综述了当前国内外航空燃气涡轮发动机燃烧室NOx发散量的控制措施以及预测方法。介绍了几个预测NOx发散量的数值模型,并对其预测结果进行了分析。     

基于分段FOX方法的民航LTO黑碳质量排放清单计算分析

根据民用航空发动机压比提出分段FOX(formation and oxidation)方法,估算民用航空发动机LTO(landing and takeoff)循环黑碳(BC)颗粒质量排放指数,结合航空发动机机场实际运行时间和燃油流量修正,编制了2018年国内某国际机场某周国内民航航班黑碳颗粒质量排放清单。结果表明:考虑燃油流量修正的分段FOX方法对民用航空发动机慢车、进近等低工况的黑碳颗粒质量估算精度较FOX方法提高1~2倍,爬升、起飞等高工况估算值更接近实验值。考虑民航实际运行时间和燃油流量后,2018年此国际机场国内民航进出港LTO循环黑碳颗粒质量周排放量约300 kg,其中B737、A320等中型机离港(起飞和爬升阶段为主)阶段排放贡献超70%。