Population growth in Bejing: trends and countermeasures

Beijing’ population has experienced a dramatic increase eversince the founding of the People’s Republic of China. Population growthin Beijing can be broadly broken down into three major components:natural increase, immigration, and the growth of floating population. Thecontinuous growth of Beijing’s population is closely linked with its centralized multi-function. The comprehensive countermeasures to control Beijing’s population growth are proposed, for example, decentralizing economicfunctions, including developing the suburbs, developing the metropolitan areaand creating counter-magnetic centers, reforming the administrative and economic systems.     

Petrogenesis of the new lherzolitic shergottite Grove Mountains 99027: Constraints of petrography,mineral chemistry,and rare earth elements

Abstract— We report petrography, mineral chemistry, and microdistribution of rare earth elements (REE) in a new lherzolitic shergottite, Grove Mountains (GRV) 99027. The textural relationship and REE patterns of minerals suggest precipitation of cumulus olivine and chromite, followed by equilibrium crystallization of a closed system with a bulk composition of the inferred intercumulus melt. Subsolidus equilibrium temperatures of pyroxenes and olivine range from 1100 to 1210 °C, based on a two‐pyroxene thermometry and Ca partitioning between augite and olivine. Oxygen fugacity of the parent magma is 1.5–2.5 (av. 2.0 ± 0.4) log units below the quartz‐fayalite‐magnetite (QFM) buffer at 960–1360 °C, according to the olivine‐orthopyroxene‐chromite barometer. The ilmenite‐chromite barometer and thermometer show much wider ranges of oxygen fugacity (1.0–7.0 log unit below QFM) and temperature (1130–480 °C), suggesting subsolidus equilibration of the oxides at low temperatures, probably due to deep burial of GRV 99027 on Mars. The low oxygen fugacity and LREE depletion of the parent magma of GRV 99027 suggest low contamination by martian crust. Characteristics of GRV 99027 demonstrate similarity of lherzolitic shergottites, suggesting a high possibility of launch pairing or a homogeneous upper mantle of Mars if they were ejected by individual impact events. However, GRV 99027 probably experienced severe post‐shock thermal metamorphism in comparison with other lherzolitic shergottites, based on the re‐crystallization of maskelynite, the homogeneity of minerals, and the low subsolidus equilibrium temperatures between chromite and ilmenite.     

ANALYSIS OF MESOSCALE CONVECTIVE SYSTEMS OVER TIBETAN PLATEAU IN SUMMER

1INTRODUCTION In meteorological satellite cloud images, the features of Mesoscale Convective System (MCS) are shown in white bright cloud cluster, cloud band, cloud line, vorti- calcloudsystem,etc. The MCSlife cycle and spatial size usuallyvaryfrom several hours to one day and 100km to approximately 1000km, respectively. In the last two decades, it has been proven that storm and intensive con- vective weather, such as spasmodic thunderstorm and gale, tornado and short macro-precipitati…     

RHESSI Observation of Atmospheric Gamma Rays from Impact of Solar Energetic Particles on 21 April 2002

The RHESSI high-resolution spectrometer detected γ-ray lines and continuum emitted by the Earth's atmosphere during impact of solar energetic particles in the south polar region from 16:00–17:00 UT on 21 April 2002. The particle intensity at the time of the observation was a factor of 10–100 weaker than previous events when gamma-rays were detected by other instruments. This is the first high-resolution observation of atmospheric gamma-ray lines produced by solar energetic particles. De-excitation lines were resolved that, in part, come from ¹⁴N at 728, 1635, 2313, 3890, and 5106 keV, and the ¹²C spallation product at ∼ 4439 keV. Other unresolved lines were also detected. We provide best-fit line energies and widths and compare these with moderate resolution measurements by SMM of lines from an SEP event and with high-resolution measurements made by HEAO 3 of lines excited by cosmic rays. We use line ratios to estimate the spectrum of solar energetic particles that impacted the atmosphere. The 21 April spectrum was significantly harder than that measured by SMM during the 20 October 1989 shock event; it is comparable to that measured by Yohkoh on 15 July 2000. This is consistent with measurements of 10–50 MeV protons made in space at the time of the γ-ray observations.     

Variations of magnetic fields and electric currents associated with a solar flare

The high-resolution vector magnetograms obtained with the solar telescope magnetograph of the Beijing Astronomical Observatory of the active region AR 4862 on 7 October, 1987, close before and after a solar flare, were used to calculate the electric current densities in the region. Then the relations between the flare and the magnetic fields as well as the electric currents were studied. The results are: (i) the transverse magnetic fields, and hence the longitudinal electric currents in the region before and after the flare, are evidently different, while the longitudinal magnetic fields remain unchanged; (ii) this confirms the result obtained previously that the flare kernels coincide with the peaks of longitudinal electric density in active regions; (iii) the close relation between the flare kernels and the electric currents indicates that the variations of the transverse magnetic fields and the longitudinal electric currents arise not from the general global evolution of the active region, but from the flare. These results tend to the conclusion that the triggering of a solar flare might be related with the plasma instability caused by the surplus longitudinal electric currents at some local regions in the solar atmosphere.     

The RHESSI Spectrometer

RHESSI observes solar photons over three orders of magnitude in energy (3 keV to 17 MeV) with a single instrument: a set of nine cryogenically cooled coaxial germanium detectors. With their extremely high energy resolution, RHESSI can resolve the line shape of every known solar gamma-ray line except the neutron capture line at 2.223 MeV. High resolution also allows clean separation of thermal and non-thermal hard X-rays and the accurate measurement of even extremely steep power-law spectra. Detector segmentation, fast signal processing, and two sets of movable attenuators allow RHESSI to make high-quality spectra and images of flares across seven orders of magnitude in intensity. Here we describe the configuration and operation of the RHESSI spectrometer, show early results on in-flight performance, and discuss the principles of spectroscopic data analysis used by the RHESSI software.     

珍珠囊发育中马氏珠母贝血清免疫因子的变化规律

马氏珠母贝育珠贝插核手术后的第1、第2、第3、第10、第15、第20、第30和第60天,抽取育珠贝血清,并研究其非特异性免疫因子酸性磷酸酶(ACP)、碱性磷酸酶(AKP)、过氧化氢酶(CAT)、超氧化物歧化酶(SOD)和溶菌酶(LSZ)的活性变化。结果表明:在珍珠囊发育初期(插核后3～10d),育珠贝血清的免疫因子ACP、AKP、CAT、SOD均比对照组(未经插核的马氏珠母贝)显著性增大(P<0.05),LSZ在插核后1～3d比对照组LSZ活性显著性增大(P<0.05);在珍珠囊发育中期(插核后第15～20天),各种免疫酶活性都逐渐降低;珍珠囊发育后期(插核30d后),育珠贝血清中的各种免疫酶活性都已恢复到对照组水平。     

海洋科技创新人才培养模式的探讨

根据海洋经济及海洋科技创新人才培养的目标 ,构建“通识教育 +专业教育 +创新教育”的人才     

鲁山棚沟金矿床包裹体特征及找矿意义

棚沟金矿床赋存于华北古陆块南缘前寒武纪花岗岩中，在空间上受区域韧性剪切带中的燕山末期花岗斑岩控制。根据矿床地质特点判断属中低温热液型金矿。通过岩石矿物组合及包裹体组成、性质、同位素等测试，确定成矿物质来源于围岩，成矿流体来源于变质水且有岩浆水与雨水的混入。通过电子探针测定的岩矿组分，计算围岩成岩及变质温度，以及成矿温度、压力和沉淀条件，认为金矿床的成矿作用，主要表现为减压环境中的岩浆热液充填和交代蚀变，以及热液的泡腾作用。从找矿标志角度确定富ＣＯ２的泡腾包裹体群、液相高硫富ＨＣＯ－３、气相高ＣＯ２和高ＣＯ２／Ｈ２Ｏ比值等参数是寻找此类金矿的重要标志     

塔里木盆地志留纪沉积层序构成及充填响应特征

塔里木盆地志留系是由角度不整合面所限定的一个区域性（二级）的沉积层序,其内可划分出5个三级沉积层序。总体上显示一个从水进到水退的沉积旋回,可识别出曲流河三角洲—辫状河三角洲、滨外陆棚及较深水盆地、无障壁碎屑滨岸—无障壁碎屑潮坪沉积体系组合,它们代表了二级沉积层序中相对低位、海侵和高位的3个沉积体系组合。研究区构造、沉积、古生物和古气候资料表明,层序1底界面和层序5顶界面是塔里木周缘板块构造挤压、盆地隆升作用的结果;层序2底界面是周缘板块强烈挤压、盆地挠曲下降作用结果,同期全球海平面快速上升;层序3、层序4和层序5的底界面是在构造作用稳定、全球海平面下降背景之上由相对海平面次一级旋回变化形成的,是古气候变化、沉积物供给及构造沉降共同作用的结果。