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.     

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。     

自适应双层网格的空间索引研究

空间数据索引是GIS系统中的关键技术,针对目前主流的网格空间索引方法进行了充分的研究比较,指出了网格索引方法对空间要素进行索引是高效的,但对于非规则地图它是不适应的.在此基础上设计了一种新的空间索引的方法,即自适应双层网格索引.详细地介绍了这种模型的实现过程,并且用实验充分论证了这个模型的效率,认为利用自适应双层网格索引检索空间数据时,处理、查询效率和占用空间等各方面具有较大优势.     

北京地区Landsat 8 OLI高空间分辨率气溶胶光学厚度反演

卫星气溶胶光学厚度(AOD)反演中,传统暗目标方法在反射率较低的水体、浓密植被覆盖区域取得了较好效果,在反射率较高且结构复杂的高反射地表上空目前多采用深蓝算法,但存在空间分辨率较低,对细节分布描述性较差等问题。为解决这一问题,本文首先以5年(2008年—2012年)长时间序列MODIS地表反射率产品为基础,采用最小值合成法建立500 m分辨率逐月地表反射率产品数据集,然后利用地物波谱库中典型地物波谱数据,分析建立MODIS与Landsat 8 OLI传感器蓝光波段反射率转换模型,最后北京地区AERONET地基观测数据确定了气溶胶光学物理参数,并反演获取了北京地区上空500 m分辨率的AOD分布。为验证反演算法的精度,分别将反演结果同AERONET及MODIS/Terra气溶胶产品(MOD04)进行交叉对比,同时利用相关系数R,均方根误差RMSE,平均绝对误差MAE以及MODIS AOD产品预期误差EE共4个指标进行衡量。结果表明:算法反演获取的AOD与AERONET观测值具有较高的一致性,各指标分别为R=0.963,RMSE=0.156,MAE=0.097,EE=85.3%,稍优于MOD04产品(R=0.962,RMSE=0.158,MAE=0.101,EE=75.8%),并且有效的对比点数也高于MOD04。通过与地基观测相比,卫星遥感获取的高分辨率城市地区AOD精度可作为定量评估城市空气质量的有效依据。     

Calibration of Infrared Absorption Coefficients for Structural Hydroxyl in Garnet by a Combined Study of Isotope Ratio Spectrometry and Vibrational Spectroscopy

An accurate determination of water content in garnet is critical to quantify the transport of water to the deep mantle by the subducted oceanic crust beyond the breakdown of hydrous phases. Fourier transform infrared spectroscopy (FTIR) is the most widely used approach to determine the species and contents of water in garnet. Accurate quantification of OH in garnet requires independent calibration using an external method, as OH absorbance is mineral and composition specific. To obtain the infrared absorption coefficients of structural hydroxyl in garnet, a combined study of spectrometric analyses by FTIR and a method combining a thermal conversion elemental analyser with isotope ratio mass spectrometry (TC/EA-MS) was carried out for fourteen gem-quality natural garnet crystals with variable compositions. The obtained molar absorption coefficients were 9322 ± 338 and 240 ± 26 l mol⁻¹ cm⁻² for grossular- and spessartine-rich garnet and pyrope-almandine garnet, respectively. These results are within the range of previous studies. A new molar absorption coefficient of 689 ± 177 l mol⁻¹ cm⁻² was obtained for pyrope-spessartine garnet. The large variation in the absorption coefficient indicates it is controlled by both garnet composition and OH-absorption bands. The obtained absorption coefficients are only appropriate for certain types of eclogitic garnet, and more studies should be carried out on eclogitic garnets.