John Turnbull Thomson,Fellow of the Royal Geographical Society: An early New Zealand geographer

John Turnbull Thomson is more known in New Zealand for his work as Chief Surveyor of Otago Province (1856–1876) and first Surveyor General of New Zealand (1877–1879). He was also a Fellow of the Royal Geographical Society of London from 1848 until his death in 1884. Thomson was an important and early self‐declared ‘does’ of geographer in New Zealand, prior to the establishment of university geography in 1937. Thomson's contribution included survey and mapping but he also gave public lectures on geography and contributed to debates about glaciation.     

基于J2ME的像素级扩展图形旋转算法的研究与实现

主要研究现有大多数平台下多图像旋转的处理,分析其中的不足之处,总结以往对图像处理方面的资料,分析得出了对图像旋转处理进行二次开发的可行,最终设计实现了一种利用三角函数对图像进行像素级旋转处理,来实现对图像的任意角度的旋转。     

基于ArcIMS与J2EE城市信息发布系统的设计与应用

介绍了基于ArcIMS和J2EE体系结构集成开发城市信息发布系统的总体框架设计、数据库设计和系统功能设计,并采用此设计方案实现了一个具体实例。     

垦利碱蓬Suaeda kenliensis J.W.Xing sp.nov.——碱蓬属一新种

报道了中国碱蓬属植物一新种——垦利碱蓬Suaeda kenliensis J.W.Xing sp.nov.。该种与南方碱蓬Suaeda australis(R.Br.)Moq.相近,但系一年生,种子具圆盘状和卵形两种形状,直径约2～3mm,叶长可达5～7 cm,无不定根,与南方碱蓬相区别。垦利碱蓬生长于潮间带和海水周期性淹没处。耐高盐,区域内海水盐度为25,滩涂表层含盐量在退潮后经日晒蒸发可达60‰以上。常形成单一种群的红海滩植被景观。模式标本存:中国科学院海洋生物标本馆;编号:MBM286537。采集地:莱州湾垦利海域潮间带泥滩。采集人:邢军武、曲宁、钟芳。     

XTE J1550-564 2001年“迷你爆发”的X射线能谱研究

黑洞X射线暂现源的迷你爆发是一类峰值光度较低、持续时间较短的爆发.由于观测数据较少,其物理机制仍不清楚.利用RXTE (Rossi X-ray Timing Explorer)卫星从2001年1月28日到3月14日的数据,研究了黑洞X射线暂现源XTE J1550–564 2001年迷你爆发的X射线能谱特性.发现在本次迷你爆发中, XTE J1550–564的X射线能谱可以用幂律谱很好地拟合.整个爆发的硬度强度图不是标准的q型,而是一直保持在最右侧.此外,还分析了此次爆发谱指数Γ与未吸收的2–10 keV能段的X射线流量F_(2–10 keV)的相关性,发现Γ-F_(2–10 keV)呈反相关关系,且谱指数Γ∈[1.35, 1.72].上述结果表明2001年这次爆发一直处于低/硬态,它的X射线辐射主要来自于辐射低效的吸积模式,如ADAF(Advection-Dominated Accretion Flow).     

基于J2EE和ArcIMS的地质灾害危险性评估项目备案系统

本文对J2EE和ArcIMS的地质灾害危险性评估项目备案系统的总体框架结构、系统三层体系结构、模块化思想设计要点和实现的技术路线及关键技术。系统应用Struts技术、数据库技术、ArcIMS的WebGIS技术和网络技术,建立了通用地理信息功能与地质灾害危险性评估项目备案自动审批的分布式软件系统,实现了地质灾害危险性评估项目备案的自动审批、管理、分析、决策、发布的一体化平台。该系统为有关部门提供辅助决策支持和信息发布服务。     

新的引潮位完全展开

Doodson进行引潮位展开时的原始数据采自Brown及Newcomb表,其黄赤交角系采用1900年1月1日之值。目前Brown系数已重新计算,黄赤交角每世纪相对变化5×10^{-4;地球轨道偏心率每世纪相对变化25×10-4。由此引起的潮波振幅长趋势变化已可辨别,这就是所谓潮波振幅的时间依赖问题。作者采用EJC表及2000.0年的黄赤交角和地球轨道偏心率数值,重新用计算机演绎了引潮位展开式,解决了时间依赖问题。文中给出了属于J2000.0系统的引潮位完全展开表。}     

A search for optical polarization from the narrow-line Seyfert 1 galaxy RE J1034+396

We present spectropolarimetry data on RE J1034+396, an ultra-soft X-ray narrow-line Seyfert 1 galaxy, and find an upper limit of ∼ 0.4 to the linear polarization in the optical band. This suggests that there is no synchrotron emission in this AGN, and thus it is unlikely that RE J1034+396 is related to BL Lac objects. Furthermore, any other polarization arising from transmission through dust, or reflection from dust and electrons, must be cancelled out by geometrical effects or diluted to a high degree by unpolarized radiation.     

Spectroscopic observations of the eclipsing polar MN Hya (RX J0929–24)

We present low–medium resolution optical spectroscopy of the eclipsing AM Her system MN Hya (RX J0929–24). We determine the magnetic field strength at the primary accretion region of the white dwarf to be 42 MG from the spacing of cyclotron features visible during π ∼ 0.4–0.7. From spectra taken during the eclipse we find that the secondary has an M3–4 spectral type. Combined with the eclipse photometry of Sekiguchi, Nakada &38; Bassett and an estimate of the interstellar extinction we find a distance of ∼300–700 pc. We find unusual line variations at π ∼ 0.9: Hα is seen in absorption and emission. This is at the same point in the orbital phase at which a prominent absorption dip is seen in soft X-rays.     

A timing formula for main-sequence star binary pulsars

In binary radio pulsars with a main-sequence star companion, the spin-induced quadrupole moment of the companion gives rise to a precession of the binary orbit. As a first approximation one can model the secular evolution caused by this classical spin-orbit coupling by linear-in-time changes of the longitude of periastron and the projected semi-major axis of the pulsar orbit. This simple representation of the precession of the orbit neglects two important aspects of the orbital dynamics of a binary pulsar with an oblate companion. First, the quasiperiodic effects along the orbit, owing to the anisotropic 1/ r ³ nature of the quadrupole potential. Secondly, the long-term secular evolution of the binary orbit, which leads to an evolution of the longitude of periastron and the projected semi-major axis, which is non-linear in time.   In this paper a simple timing formula for binary radio pulsars with a main-sequence star companion is presented which models the short-term secular and most of the short-term periodic effects caused by the classical spin-orbit coupling. I also give extensions of the timing formula that account for long-term secular changes in the binary pulsar motion. It is shown that the short-term periodic effects are important for the timing observations of the binary pulsar PSR B1259–63. The long-term secular effects are likely to become important in the next few years of timing observations of the binary pulsar PSR J0045–7319. They could help to restrict or even determine the moments of inertia of the companion star and thus probe its internal structure.   Finally, I reinvestigate the spin-orbit precession of the binary pulsar PSR J0045–7319 since the analysis given in the literature is based on an incorrect expression for the precession of the longitude of periastron. A lower limit of 20° for the inclination of the B star with respect to the orbital plane is derived.