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961.
提出在不规则多边形面积统计汇总工作中应用基于Auto CAD扩展属性的技术,对多边形的对象属性进行存储,将多边形图形数据与属性数据一体化结合,实现了多边形图形多元化处理,如统计分析、汇总报表、图形标注等的自动化、智能化,为不规则多边形面积处理提出了一种较新的处理思路。本文结合工程实例,通过对比分析详细介绍了该技术的具体应用过程。 相似文献
962.
在城市森林建设管理中充分利用3S技术对空间信息的快速获取、存储、分析优势,可以大大提高城市森林的建设质量与效率。本论文分析了城市森林建设各阶段对3S技术的应用需求,并以太原城郊森林公园的建设管理为例,阐述相关技术路线与应用形式。 相似文献
963.
964.
对汶川大地震后北川县唐家山堰塞湖区域的地形地貌、土地质量、植被覆盖、工程建设及生态环境等基本情况进行详细调研,运用RS,GIS等技术结合景观格局指数分析法,对唐家山堰塞湖区域的整体景观生态格局指标进行研究,分析唐家山堰塞湖区域内斑块和廊道等景观格局因子的变化数据,总结区域内景观生态格局的各类特征,为地震灾区生态修复及环境破坏评价提供参考. 相似文献
965.
966.
R. Barnard S. B. Foulkes C. A. Haswell U. Kolb J. P. Osborne J. R. Murray 《Monthly notices of the Royal Astronomical Society》2006,366(1):287-294
We present results from three XMM–Newton observations of the M31 low mass X-ray binary (LMXB) XMMU J004314.4+410726.3 (Bo 158), spaced over 3 d in 2004 July. Bo 158 was the first dipping LMXB to be discovered in M31. Periodic intensity dips were previously seen to occur on a 2.78-h period, due to absorption in material that is raised out of the plane of the accretion disc. The report of these observations stated that the dip depth was anticorrelated with source intensity. In light of the 2004 XMM–Newton observations of Bo 158, we suggest that the dip variation is due to precession of the accretion disc. This is to be expected in LMXBs with a mass ratio ≲0.3 (period ≲4 h), as the disc reaches the 3:1 resonance with the binary companion, causing elongation and precession of the disc. A smoothed particle hydrodynamics simulation of the disc in this system shows retrograde rotation of a disc warp on a period of ∼11 P orb , and prograde disc precession on a period of 29 ± 1 P orb . This is consistent with the observed variation in the depth of the dips. We find that the dipping behaviour is most likely to be modified by the disc precession, hence we predict that the dipping behaviour repeats on an 81 ± 3 h cycle. 相似文献
967.
Michael D. Audley † Fumiaki Nagase Kazuhisa Mitsuda Lorella Angelini Richard L. Kelley 《Monthly notices of the Royal Astronomical Society》2006,367(3):1147-1154
We report on two ASCA observations of the high-mass X-ray binary pulsar OAO 1657−415. A short observation near mid-eclipse caught the source in a low-intensity state, with a weak continuum and iron emission dominated by the 6.4-keV fluorescent line. A later, longer observation found the source in a high-intensity state and covered the uneclipsed through mid-eclipse phases. In the high-intensity state, the non-eclipse spectrum has an absorbed continuum component due to scattering by material near the pulsar and 80 per cent of the fluorescent iron emission comes from less than 19 light-second away from the pulsar. We find a dust-scattered X-ray halo whose intensity decays through the eclipse. We use this halo to estimate the distance to the source as 7.1 ± 1.3 kpc. 相似文献
968.
The term 'dynamo' means different things to the laboratory fusion plasma and astrophysical plasma communities. To alleviate the resulting confusion and to facilitate interdisciplinary progress, we pinpoint conceptual differences and similarities between laboratory plasma dynamos and astrophysical dynamos. We can divide dynamos into three types: 1. magnetically dominated helical dynamos which sustain a large-scale magnetic field against resistive decay and drive the magnetic geometry towards the lowest energy state, 2. flow-driven helical dynamos which amplify or sustain large-scale magnetic fields in an otherwise turbulent flow and 3. flow-driven non-helical dynamos which amplify fields on scales at or below the driving turbulence. We discuss how all three types occur in astrophysics whereas plasma confinement device dynamos are of the first type. Type 3 dynamos require no magnetic or kinetic helicity of any kind. Focusing on Types 1 and 2 dynamos, we show how different limits of a unified set of equations for magnetic helicity evolution reveal both types. We explicitly describe a steady-state example of a Type 1 dynamo, and three examples of Type 2 dynamos: (i) closed volume and time dependent; (ii) steady state with open boundaries; (iii) time dependent with open boundaries. 相似文献
969.
970.
Modern spectropolarimeters are capable of detecting subkilogauss field strengths using the Zeeman effect in line profiles from the static photosphere, but supersonic Doppler broadening makes it more difficult to detect the Zeeman effect in the wind lines of hot stars. Nevertheless, the recent advances in observational capability motivate an assessment of the potential for detecting the magnetic fields threading such winds. We incorporate the weak-field longitudinal Zeeman effect in the Sobolev approximation to yield integral expressions for the flux of circularly polarized emission. To illustrate the results, two specific wind flows are considered: (i) spherical constant expansion with v ( r ) = v ∞ and (ii) homologous expansion with v ( r ) ∝ r . Axial and split monopole magnetic fields are used to schematically illustrate the polarized profiles. For constant expansion, optically thin lines yield the well-known 'flat-topped' total intensity emission profiles and an antisymmetric circularly polarized profile. For homologous expansion, we include occultation and wind absorption to provide a more realistic observational comparison. Occultation severely reduces the circularly polarized flux in the redshifted component, and in the blueshifted component, the polarization is reduced by partially offsetting emission and absorption contributions. We find that for a surface field of approximately 100 G, the largest polarizations result for thin but strong recombination emission lines. Peak polarizations are approximately 0.05 per cent, which presents a substantial although not inconceivable sensitivity challenge for modern instrumentation. 相似文献