1：100万图号中行号、列号正误的快速判断方法     

王宝生  顾栋材 《现代测绘》2009,32(4):24-25

针对多个县(市)、区土地调查文字材料将1:100万图号中的行、列号用错而产生严重缺陷的事实,本人认真学习了"国家基本比例尺地形图分幅和编号"的基础知识,并总结归纳出简易的快速判断正误的方法,以杜绝类似差错的发生.  相似文献   

Chandra observations of Comet 9P/Tempel 1 during the Deep Impact campaign     

C.M. Lisse  K. Dennerl  S.J. Wolk  T.H. Zurbuchen  R. Hoekstra  C.D. Fry  T. Mäkinen 《Icarus》2007,190(2):391-405

We present results from the Chandra X-ray Observatory's extensive campaign studying Comet 9P/Tempel 1 (T1) in support of NASA's Deep Impact (DI) mission. T1 was observed for ∼295 ks between 30th June and 24th July 2005, and continuously for ∼64 ks on July 4th during the impact event. X-ray emission qualitatively similar to that observed for the collisionally thin Comet 2P/Encke system [Lisse, C.M., Christian, D.J., Dennerl, K., Wolk, S.J., Bodewits, D., Hoekstra, R., Combi, M.R., Mäkinen, T., Dryer, M., Fry, C.D., Weaver, H., 2005b. Astrophys. J. 635 (2005) 1329-1347] was found, with emission morphology centered on the nucleus and emission lines due to C, N, O, and Ne solar wind minor ions. The comet was relatively faint on July 4th, and the total increase in X-ray flux due to the Deep Impact event was small, ∼20% of the immediate pre-impact value, consistent with estimates that the total coma neutral gas release due to the impact was 5×¹⁰⁶ kg (∼10 h of normal emission). No obvious prompt X-ray flash due to the impact was seen. Extension of the emission in the direction of outflow of the ejecta was observed, suggesting the presence of continued outgassing of this material. Variable spectral features due to changing solar wind flux densities and charge states were clearly seen. Two peaks, much stronger than the man-made increase due to Deep Impact, were found in the observed X-rays on June 30th and July 8th, 2005, and are coincident with increases in the solar wind flux arriving at the comet. Modeling of the Chandra data using observed gas production rates and ACE solar wind ion fluxes with a CXE mechanism for the emission is consistent, overall, with the temporal and spectral behavior expected for a slow, hot wind typical of low latitude emission from the solar corona interacting with the comet's neutral coma, with intermittent impulsive events due to solar flares and coronal mass ejections.  相似文献   

一个基于AOP的Bean锁算法   总被引：1，自引：1，他引：0  

黄强  李敏  楼新远 《成都信息工程学院学报》2006,21(2):225-228

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。  相似文献   

双经纬仪虚拟像坐标二维直接定位     

陈基伟 《大地测量与地球动力学》2006,26(2):87-90

提出了一种基于虚拟左、右像片像空间坐标系的二维直接定位法,可快速提取工业测量系统两台经纬仪之间的相对定位元素并完成相对定位。它不用进行迭代,既可以在右测站的定位元素未知时进行定位元素的解算,又具有简单清楚的几何意义。最后用算例对算法进行了验证。  相似文献   

An ultraluminous X-ray microquasar in NGC 5408?     

R. Soria  R. P. Fender  D. C. Hannikainen  A. M. Read  I. R. Stevens 《Monthly notices of the Royal Astronomical Society》2006,368(4):1527-1539

We studied the radio source associated with the ultraluminous X-ray source in NGC 5408  ( L _X≈ 10⁴⁰ erg s⁻¹)  . The radio spectrum is steep (index  ≈−1  ), consistent with optically thin synchrotron emission, not with flat-spectrum core emission. Its flux density (≈0.28 mJy at 4.8 GHz, at a distance of 4.8 Mpc) was the same in the March 2000 and December 2004 observations, suggesting steady emission rather than a transient outburst. However, it is orders of magnitude higher than expected from steady jets in stellar-mass microquasar. Based on its radio flux and spectral index, we suggest that the radio source is either an unusually bright supernova remnant, or, more likely, a radio lobe powered by a jet from the black hole (BH). Moreover, there is speculative evidence that the source is marginally resolved with a radius ∼30 pc. A faint H  ii region of similar size appears to coincide with the radio and X-ray sources, but its ionization mechanism remains unclear. Using a self-similar solution for the expansion of a jet-powered electron–positron plasma bubble, in the minimum-energy approximation, we show that the observed flux and (speculative) size are consistent with an average jet power  ≈ 7 × 10³⁸ erg s⁻¹∼ 0.1 L _X∼ 0.1 L _Edd  , an age ≈10⁵ yr, a current velocity of expansion ≈80 km s⁻¹. We briefly discuss the importance of this source as a key to understand the balance between luminosity and jet power in accreting BHs.  相似文献   

Intermediate mass black holes in accreting binaries: formation, evolution and observational appearance     

Simon F. Portegies Zwart  Jasinta Dewi  Tom Maccarone 《Monthly notices of the Royal Astronomical Society》2004,355(2):413-423

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Quenched millimetre emission from Cygnus X-1 in a soft X-ray state     

S. P. Tigelaar  R. P. Fender  R. P. J. Tilanus  E. Gallo  G. G. Pooley 《Monthly notices of the Royal Astronomical Society》2004,352(3):1015-1018

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JXTA安全问题研究     

张莹  徐志根 《成都信息工程学院学报》2004,19(4):496-499

P2P对等网络(Peer-to-Peer network)是近年来引起广泛关注的网络技术,JXTA项目则是构建P2P网络平台的一个典型例子.针对JXTA网络中面临的安全问题及解决方案进行了初步探讨,最后以在JXTA中实现数字签名为例,介绍了目前正在积极开发中的JXTA安全项目.  相似文献   

设计模式及其在J2ME中的应用   总被引：2，自引：0，他引：2  

韩鹏  李成忠 《成都信息工程学院学报》2004,19(3):332-335

设计模式被描述为在一定的环境中解决某一类问题的方案.已成为现代软件系统设计的重要研究对象.介绍了J2ME体系结构,并深入探讨了3种典型设计模式在J2ME开发中的应用.  相似文献   

On the X-ray time-lags in the black hole candidates     

O. Kotov  E. Churazov  M. Gilfanov 《Monthly notices of the Royal Astronomical Society》2001,327(3):799-807

It is shown that the energy dependence of the time-lags in Cygnus X-1 excludes any significant contribution of the standard reflected component to the observed lags. The conclusion is valid in the     frequency range where time-lags have been detected with sufficient significance. In fact, the data hint that the reflected component is working in the opposite direction, reducing the lags at energies where the contribution of the reflected component is significant.
We argue that the observed logarithmic dependence of time-lags on energy could be due to the small variations of the spectral index in the frame of a very simple phenomenological model. We assume that an optically thin flow/corona, emitting a power law like spectrum, is present at a range of distances from the compact object. The slope of the locally emitted spectrum is a function of distance, with the hardest spectrum emitted in the innermost region. If perturbations with different time-scales are introduced to the accretion flow at different radii, then X-ray lags naturally appear, caused by the inward propagation of perturbations on the diffusion time-scales.  相似文献