社旗县土地整理帮农民走上致富路

近年来,社旗县把土地开发整理与建设社会主义新农村结合起来,把土地开发整理与农业内部结构调整发展高效农业结合起来,把土地开发整理与扶贫解困脱贫致富结合起来,使之成为实实在在的富民工程、民心工程。     

关于太阳底部贯穿对流区的延伸程度

众所周知 ,贯穿对流对恒星演化有至关重要的影响 .然而至今对此问题尚无完善的理论处理方法 .尽管该问题已经取得了很大的进展[1-4 ] ,但在恒星演化计算中处理贯穿对流最广泛的仍是某种唯象的混合长理论[5,6] .日震学提供了一个探测太阳内部结构的强有力手段 ,它对恒星对流理论给出了一个严格的限制 .　　在过去几年中 ,利用日震方法探测太阳对流区之下贯穿对流区的结构引起了人们的特别关注 .所有的理论研究都是根据这样一种简单的唯象贯穿对流模型[5-9] :在稍许高于绝热温度梯度的对流区的下方 ,紧贴着的是一个稍许低于绝热温度梯度的贯穿…     

Early Development of Silvetia babingtonii （Fucales,Phaeophyceae）

Silvetia babingtonii is a potentially economic brown alga for sources of food and high-value added utilization.So far,sporeling nursery and field cultivation has not been successful.The lack of knowledge on development and life cycle of this alga hinder the development of techniques for the sporeings and cultivation.In this study,internal structure of oogonium and antherium of S.babingtonii was observed with hematoxylin and eosin staining and through microscope.Meanwhile,early development from zygotes to juvenile sporelings was studied at 20℃ under 60-100 μmol photons m^-2 s^-1.Zygotes germinated and divided into thallus and rhizoid cells.The larger thallus cells further divided and developed into juvenile sporelings; while the smaller rhizoid cells divided and elongated into rhizoid hairs.These findings documented the life cycle ofS.babingtonii and provided fundamental knowledge for sporeling nursery in the near future.     

接收函数方法在新疆和田地震台阵的应用研究

自20世纪80年代以来,远震体波接收函数已经开始广泛地应用于地球内部结构的研究中,它是现阶段国内外探测地壳及上地幔结构和间断面起伏特征的重要手段.在接收函数应用研究中,对于宽频带地震台站接收函数的稳定性和台站下方的结构已有许多成果,而对短周期地震台站接收函数的稳定性和可靠性分析很少.     

四川地区地震精定位

地震定位是地震学中最经典、最基本的问题之一,对于研究地震活动构造、地球内部结构、震源的几何构造等地震学中的基本问题有重要意义.随着区域地震台网的密度不断提高,记录到同一地震的台站也越来越多,地震定位精度也越来越高.     

地震波三维Q值成像

品质因子Q通常可表述为频率f的函数:Q(f)=Q0fa.由于地震波能提供地球内部物质组成、晶体结构和物态、温度以及物质流动等信息,且地震波在地球介质中的衰减与Q值直接相关,因此,通过地震波研究地球介质Q值,已经成为研究地球内部结构及其动力系统的重要手段.     

Dome Argus： Ideal site for deep ice drilling

Located on the centre of ice drainage range, the highest Dome Argus （Dome A） of East Antarctic Ice Sheet （EAIS）, could be represented as an ideal site for deep ice cores drilling containing oldest paleo-climate records. To select a suitable drilling site for deep ice core, it needs gather all information pertaining to the local meteorology, ice sheet landforms, ice thickness, subgla- cial topography of bed rocks, ice velocity, internal structures of ice sheet, etc. Based on the International Partnerships in Ice Core Sciences （IPICS）, we present recent achievement of glaciological research and its perspective at Dome A in this paper. We system- atically discussed the merits and possible ventures of potential drilling sites around Dome A. Among all the candidates, we find that the Chinese Antarctic Kunlun Station is the best site for and assess further the possibility to obtain a replicate core for carrying out the first deep ice core drilling campaign. We emphasize studying dynamics and evolution of climate change.     

地震基本知识问答

1．地球的内部结构是什么？ 答：地球的最外层叫地壳;地壳下面的部分叫地幔;地球最中心的部分叫地核。地球的平均半径为6370公里左右,地壳厚度为35公里左右,大多数破坏性地震就发生在地壳内。 2．地球表面是由什么组成的？     

Radio Luminosity, Black Hole Mass and Eddington Ratio for Quasars from the Sloan Digital Sky Survey

We investigate the MBH-O'.relation for radio-loud quasars with redshift z＜0.83 in Data Release 3 of the Sloan Digital Sky Survey (SDSS).The sample consists of 3772 quasars with better models of the H/~ and [O III] lines and available radio luminosity,including 306 radio-loud quasars,3466 radio-quiet quasars with measured radio luminosity or upper-limit of radio luminosity (181 radio-quiet quasars with measured radio luminosity).The virial supermassive black hole mass (MBH) is calculated from the broad H/line,and the host stellar velocity dispersion (σ*) is traced by the core [O III] gaseous velocity dispersion.The radio luminosity and radio loudness are derived from the FIRST catalog.Our results are as follows:(1) For radio-quiet quasars,we confirm that there is no obvious deviation from the MBH-O".relation defined for inactive galaxies when the uncertainties in MBH and the luminosity bias are concerned.(2) We find that the radio-loud quasars deviate more from the MBH-σ.relation than do the radio-quiet quasars.This deviation is only partly due to a possible cosmological evolution of the MBH-σ* relation and the luminosity bias.(3) The radioluminosity is proportional to M128 0.23-0.16 BH(LBol/LEdd)1.29 0.31-0.24 for radio-quiet quasars and to M3.10 0.6.-0.70(LBol.LEdd)4.18 1.40-1.10 for radio-loud quasars.The weaker dependence of the radio luminosity on the mass and the Eddington ratio for radio-loud quasars shows that other physical effects would account for their radio luminosities,such as the spin of the black hole.