STATISTICAL ANALYSIS ON THE INFLUENCE OF THE LANDFALLING STRONG TROPICAL CYCLONES IN THE CATASTROPHIC MIGRATIONS OF NILAPARVATA LUGENS(STL) IN CHINA

In order to clarify the statistical pattern by which landfalling strong tropical cyclones(LSTCs)influenced the catastrophic migrations of rice brown planthopper(BPH),Nilaparvata lugens(stl)in China,the data of the LSTCs in China and the lighting catches of BPH that covered the main Chinese rice-growing regions from 1979 to 2008 were collected and analyzed in this work with the assistance of ArcGIS9.3,a software of geographic information system.The results were as follows:(1)In China,there were 220 strong tropical cyclones that passed the main rice-growing regions and 466 great events of BPH’s immigration in the 30 years from 1979 to 2008.73 of them resulted in the occurrence of BPH’s catastrphic migration(CM)events directly and 147 of them produced indirect effect on the migrations.(2)The number of the LSTCs was variable in different years during 1979 to 2008 and their influence was not the same in the BPH’s northward and southward migrations in the years.In the 30 years,the LSTCs brought more obvious influence on the migrations in 1980,1981,2005,2006 and 2007.The influence was the most obvious in2007 and all of the 7 LSTCs produced remarkable impact on the CMs of BPH’s populations.The effect of the LSTCs on the northward immigration of BPH’s populations was the most serious in 2006 and the influence on the southward immigration was the most remarkable in 2005.(3)In these years,the most of LSTCs occurred in July,August and September and great events of BPH's immigration occurred most frequently in the same months.The LSTCs played a more important role on the CM of BPH’s populations in the three months than in other months.(4)The analysis on the spatial distribution of the LSTCs and BPH’s immigration events for the different provinces showed that the BPH’s migrations in the main rice-growing regions of the Southeastern China were influenced by the LSTCs and the impact was different with the change of their spatial probability distribution during their passages.The most serious influence of the LSTCs on the BPH’s migrations occurred in Guangdong and Fujian provinces.(5)The statistical results indicated that a suitable insect source is an indispensable condition of the CMs of BPH when a LSTC influenced a rice-growing region.     

东疆红山Cu-Au矿床氧化带硫酸盐矿物穆斯堡尔谱特征及其意义

穆斯堡尔谱对确定铁离子占位、核外环境及氧化态方面有着独特的优势。在红山铜金矿床氧化带硫酸盐矿物的XRD、TA、湿法化学分析和红外光谱测试的基础上,测定了板铁矾、针绿矾等8种硫酸盐矿物的室温57Fe穆斯堡尔谱,并根据常温下硫酸盐矿物穆斯堡尔谱参数和其晶体结构中Fe3+和Fe2+的占据位置对其谱峰进行了指派。结果表明本矿床氧化带硫酸盐矿物的穆斯堡尔谱的同质异能位移较小、四级矩分裂值分布范围较大、无磁超精细分裂等特征,且硫酸盐矿物结构中存在着共价键。通过与青海锡铁山铅锌矿氧化带硫酸盐矿物的穆斯堡尔谱相比较,两者在近地表风化及氧化过程中所处的物理化学条件基本相同,酸性和氧化性的环境为硫酸盐矿物的产生和保存提供了良好条件,但红山矿床更为干旱少雨,导致两者硫酸盐的穆斯堡尔谱参数略有不同。     

麻江古油藏油源识别与油气运聚分析：来自油气地球化学的证据

充分考虑热演化过程中烃源岩干酪根、族组分、固体沥青及正构烷烃碳同位素相互关系及变化规律,通过地球化学分析并结合前人碳同位素及芳烃标志物研究进行综合分析,结果表明古油藏各区域储层早期均存在下寒武统黑色泥岩来源,后期来源有较大差别,麻江古背斜以南各地沥青均不同程度与中寒武统都柳江组有关,北凯里液态原油及油苗为五峰组及龙马溪组印支期成藏产物,其保存环境为储层早期成岩过程中形成的独立封闭系统。在油源识别的基础上,结合构造地质背景、油气成藏条件及流体活动规律分析,认为黔南坳陷及邻区下寒武统、都柳江组、五峰组及龙马溪组烃源岩的分布控制了该区油气富集规律,黔南海西期断裂系统与加里东运动形成的不整合面构成不同期次油气运聚的输导系统,海西期形成的一系列正断裂是麻江古油藏成藏的关键。     

Characteristics of the supernova remnant G351.7+0.8 and a distance argument against its association with PSR J1721−3532

New images of the supernova remnant (SNR) G351.7+0.8 are presented based on 21-cm H  i -line emission and continuum emission data from the Southern Galactic Plane Survey. SNR G351.7+0.8 has a flux density of 8.4 ± 0.7 Jy at 1420 MHz. Its spectral index is 0.52 ± 0.25 ( S = v ^−α) between 1420 and 843 MHz, typical of adiabatically expanding shell-like remnants. H  i observations show structures possibly associated with the SNR in the radial velocity range of −10 to −18 km s⁻¹, and suggest a distance of 13.2 kpc and a radius of 30.7 pc. The estimated Sedov age for G351.7+0.8 is less than  6.8×10⁴ yr  . A young radio pulsar PSR J1721−3532 lies close to SNR G351.7+0.8 on the sky. The new distance and age of G351.7+0.8 and recent proper motion measurements of the pulsar strongly argue against an association between SNR G351.7+0.8 and PSR J1721−3532. There is an unidentified, faint X-ray point source 1RXS J172055.3−353937 which is close to G351.7+0.8. This may be a neutron star potentially associated with G351.7+0.8.     

一个基于AOP的Bean锁算法

提出了一种基于Aspect Oriented Programming（AOP）的Bean锁算法，通过将Bean锁抽象成该问题的一个方面（Aspect），通过AOP引擎使用该算法动态生成加锁Bean，大大降低Bean锁代码的重复量，并在基本不影响性能的前提下，提高代码复用率。通过使用基于AOP的Bean锁，Bean可以完全消除锁代码，从而提高Bean代码的可维护性。     

Energy Distribution of a Gödel-Type Space–Time

We calculate the energy and momentum distributions associated with a Gödel-type space–time, using the well-known energy–momentum complexes of Landau–Lifshitz and Møller. We show that the definitions of Landau–Lifshitz and Møller do not furnish a consistent result.     

Physics of accretion in the millisecond pulsar XTE J1751 − 305

We have undertaken an extensive study of X-ray data from the accreting millisecond pulsar XTE J1751 − 305 observed by RXTE and XMM–Newton during its 2002 outburst. In all aspects this source is similar to the prototypical millisecond pulsar SAX J1808.4 − 3658, except for the higher peak luminosity of 13 per cent of Eddington, and the optical depth of the hard X-ray source, which is larger by a factor ∼2. Its broad-band X-ray spectrum can be modelled by three components. We interpret the two soft components as thermal emission from a colder  ( kT ∼ 0.6 keV)  accretion disc and a hotter (∼1 keV) spot on the neutron star surface. We interpret the hard component as thermal Comptonization in plasma of temperature ∼40 keV and optical depth ∼1.5 in a slab geometry. The plasma is heated by the accretion shock as the material collimated by the magnetic field impacts on to the surface. The seed photons for Comptonization are provided by the hotspot, not by the disc. The Compton reflection is weak and the disc is probably truncated into an optically thin flow above the magnetospheric radius. Rotation of the emission region with the star creates an almost sinusoidal pulse profile with an rms amplitude of 3.3 per cent. The energy-dependent soft phase lags can be modelled by two pulsating components shifted in phase, which is naturally explained by a different character of emission of the optically thick spot and optically thin shock combined with the action of the Doppler boosting. The observed variability amplitude constrains the hotspot to lie within 3°–4° of the rotational pole. We estimate the inner radius of the optically thick accreting disc to be about 40 km. In that case, the absence of emission from the antipodal spot, which can be blocked by the accretion disc, gives the inclination of the system as ≳70°.