国内外页岩气研究进展及山东省页岩气资源潜力

当前国际能源供需矛盾突出,能源问题日益成为各国关注的焦点,页岩气资源勘查开发备受世界瞩目;全球页岩气资源非常丰富,主要分布在北美、中亚和中国、拉美、中东和北非、前苏联地区;近年来随着开采和利用技术的不断进步,美洲、欧洲、亚洲国家对页岩气的勘查开发正在形成热潮。中国页岩气资源丰富,对页岩气的区域勘查研究越来越多,取得了不错的成果,但总体上中国页岩气的研究和勘查尚处于起步阶段,同时中国的开发技术与国外相比还存在较大的差距。结合山东省不同类型富含有机质泥页岩的具体特点和国内外页岩气勘查经验,初步认为山东省具有一定的页岩气形成条件,山东省页岩气远景区地层主要为新生代古近纪济阳群和五图群及官庄群,中生代早白垩世莱阳群,古生代石炭—二叠纪月门沟群和石盒子群;在综合考虑页岩的赋存层位、页岩成气潜力和页岩气开发可行性的基础上,提出了山东省页岩气潜力区为:济阳坳陷区、临清坳陷区、胶莱坳陷区和黄县(龙口)凹陷以及鲁西南潜隆起区,其中济阳-临清坳陷地区页岩气潜力较好。     

湖北省棉花产量的变化与棉田布局的战略调整*

本文揭示了湖北省棉花亩产的增长具有北高南低的特点,分析了鄂北地区种植棉花的自然优势和经济效盆大于江汉平原,从而提出湖北省棉花北移的战略调整的设想。     

复杂风况条件下戈壁输沙量变化规律的研究

 戈壁输沙量与输沙势的定量关系一直是风沙地貌及风沙工程的关键科学问题之一。对莫高窟顶戈壁输沙量的长期监测（2008年5月至2009年4月）结果表明,窟顶戈壁输沙势为129VU,窟顶北侧的总输沙量约905 kg·m-1左右。其中,偏东风输沙量达500 kg·m-1,偏西风输沙量达320 kg·m-1。当风速大于11 m·s-1时,戈壁风沙发生长距离的输送,偏西风可将265 kg·m-1的沙量输送到窟区,偏东风可将410 kg·m-1的沙量吹回到鸣沙山。根据本区偏东风强盛,且偏东风戈壁输沙量大于偏西风输沙量的特点,提出了以固为主,输导结合的莫高窟风沙防治的主导思路。认为在窟顶构建一个既能阻截沙物质,又能对阻截的沙物质进行输导的人工戈壁床面是完全可行的。     

对废弃非金属矿山的再次开发利用的优点

随着经济发展对建筑材料的需求促使非金属矿山的开采,随着矿山矿产资源的枯竭,一些矿山面临关闭,一般闭坑矿山需投入大量资金进行恢复治理。对于废弃非金属矿山再次开发利用可节约土地资源,优化矿产资源利用,且具有良好的经济效益,因此具有良好的前景。     

Star formation in the Cepheus Flare region – II. A-type stars associated with IRAS sources

In order to reveal the star-forming history of the molecular cloud complex we studied the intermediate mass stellar population in the Cepheus Flare region. (Paper I dealt with the distance and the young stellar object candidates of the region.) Correlating the IRAS Point Source Catalogue and Faint Source Catalogue positions with those of 1214 B8–A8 and 1760 F0–F5 type stars brighter than     and classified during an objective prism survey, we identified 19 stars showing far-infrared excess emission in the Cepheus Flare region. In addition to the 16 stars whose counterparts are given in the IRAS catalogues, we found three more stars with infrared excess not recognized before. In order to identify the young medium-mass stars associated with the Cepheus Flare molecular clouds we observed the optical spectra of the IR-excess stars, and using published optical photometry and the IRAS data we examined their spectral energy distributions (SEDs) and IRAS two-colour diagram. The observations resulted in the discovery of a new Herbig Ae/Be star, BD +68°1118, coinciding with IRAS 21169+6842. More evolved HAe/Be stars may be SAO 19953, BD +67°1314 and BD +69°1231, whose H α lines showed weak emission components. Possible β Pictoris- or Vega-type stars may be HD 203854, HD 212826 and HD 216486, whereas the far-infrared fluxes at the positions of BD +72°1018, HD 210806 and HD 217903 can be attributed to the heating of the interstellar environment. We used distances and radial velocities of the stars derived from the spectroscopy and published optical photometry as indicators of their relations to the clouds. Information on the environment of the observed stars deduced from the diffuse interstellar band at λ 6613 is briefly discussed.     

Sources of SEP Acceleration during a Flare – CME Event

A high-speed, halo-type coronal mass ejection (CME), associated with a GOES M4.6 soft X-ray flare in NOAA AR 0180 at S12W29 and an EIT wave and dimming, occurred on 9 November 2002. A complex radio event was observed during the same period. It included narrow-band fluctuations and frequency-drifting features in the metric wavelength range, type III burst groups at metric – hectometric wavelengths, and an interplanetary type II radio burst, which was visible in the dynamic radio spectrum below 14 MHz. To study the association of the recorded solar energetic particle (SEP) populations with the propagating CME and flaring, we perform a multi-wavelength analysis using radio spectral and imaging observations combined with white-light, EUV, hard X-ray, and magnetogram data. Velocity dispersion analysis of the particle distributions (SOHO and Wind in situ observations) provides estimates for the release times of electrons and protons. Our analysis indicates that proton acceleration was delayed compared to the electrons. The dynamics of the interplanetary type II burst identify the burst source as a bow shock created by the fast CME. The type III burst groups, with start times close to the estimated electron-release times, trace electron beams travelling along open field lines into the interplanetary space. The type III bursts seem to encounter a steep density gradient as they overtake the type II shock front, resulting in an abrupt change in the frequency drift rate of the type III burst emission. Our study presents evidence in support of a scenario in which electrons are accelerated low in the corona behind the CME shock front, while protons are accelerated later, possibly at the CME bow shock high in the corona.     

基于多源空间数据的地质灾害监测预警系统研究——以云南省德钦县为例

三维激光扫描、合成孔径雷达干涉(InSAR)、全球导航卫星系统(GNSS)、无人机及物联网等新技术为测绘、监测以及早期预警系统(EWS)提供了更丰富的数据源。本文基于上述技术,设计提出了一种针对滑坡、泥石流等地质灾害监测预警系统(GDMEWS)的解决方案。介绍了地质灾害监测预警系统复杂多变的特点,对系统的体系结构、多源空间数据库组成、开发模式、业务逻辑、系统开发的方法及关键技术进行了分析。论文以具有独特的地形地貌、滑坡和泥石流类型众多、典型多样的德钦县为案例区,探讨GDMEWS的体系机构及关键技术。首先,对系统的功能要求,监测及预测模型等进行了讨论;其次,研究了灾前预警、灾中抢险、灾后重建全过程的逻辑关系,开发防灾减灾和地质灾害管理支持工具;再次,阐述了多源监测数据集成方法和地质灾害机理模型的建立。最后,对GDMEWS的研发实现进行了阐述,并说明其在德钦县地灾的全过程实时动态管理、监测和预警中的应用。     

滇池水体污染和治理的特点

滇池是一个发育至老年末期的高原湖泊。滇池流域是缺水地区,水资源的供需平衡靠径流、污水和农田回归水的循环利用得以实现,重复用水率25％。随着人口的增长和工农业的发展,滇池水资源污染日益加重,水体严重富营养化。滇池是整个流域污染物唯一的汇,这也是其难以治理的原因。近年来,从中央到地方用于滇池污染治理的总投资已逾40亿元,而治理措施收效甚微,因此,对滇池这样有特殊污染机理的湖泊治理应从更宽泛的角度出发去考虑,甚至采取非常措施。     

太阳软X射线观测进展

太阳软x射线观测在太阳物理的研究中，特别在日冕结构、磁场和日冕等离子体活动等物理现象的研究中起着重要的作用。太阳软x射线观测主要有光谱和成像观测两种．随着观测技术、方法和内容的发展，太阳软x射线观测揭示了太阳物理的许多重要的科学现象，并在预报、监测空间天气变化，预警空间灾变天气等方面也有着重要的应用．     

Low-mass binary-induced outflows from asymptotic giant branch stars

A significant fraction of planetary nebulae (PNe) and protoplanetary nebulae (PPNe) exhibit aspherical, axisymmetric structures, many of which are highly collimated. The origin of these structures is not entirely understood, however, recent evidence suggests that many observed PNe harbour binary systems, which may play a role in their shaping. In an effort to understand how binaries may produce such asymmetries, we study the effect of low-mass  (<0.3 M_⊙)  companions (planets, brown dwarfs and low-mass main-sequence stars) embedded into the envelope of a  3.0-M_⊙  star during three epochs of its evolution [red giant branch, asymptotic giant branch (AGB), interpulse AGB]. We find that common envelope evolution can lead to three qualitatively different consequences: (i) direct ejection of envelope material resulting in a predominately equatorial outflow, (ii) spin-up of the envelope resulting in the possibility of powering an explosive dynamo-driven jet and (iii) tidal shredding of the companion into a disc which facilitates a disc-driven jet. We study how these features depend on the secondary's mass and discuss observational consequences.