Pulsar Wind Nebulae in Egret Error Boxes

A remarkable number of pulsar wind nebulae (PWN) are coincident with EGRET γ-ray sources. X-ray and radio imaging studies of unidentified EGRET sources have resulted in the discovery of at least six new pulsar wind nebulae (PWN). Stationary PWN (SPWN) appear to be associated with steady EGRET sources with hard spectra, typical for γ-ray pulsars. Their toroidal morphologies can help determine the geometry of the pulsar which is useful for constraining models of pulsed γ-ray emission. Rapidly moving PWN (RPWN) with more cometary morphologies seem to be associated with variable EGRET sources in regions where the ambient medium is dense compared to what is typical for the ISM.     

异龙湖流域湿地生态系统健康评价

湿地生态系统健康状况评价为湿地资源的合理开发、生态系统的维护提供了重要的借鉴。在充分了解异龙湖流域湿地资源环境的基础上,结合湖泊湿地生态系统的概念及内涵,采用PSR(压力-状态-响应)框架模型和生态系统健康指数计算方法对研究区湿地生态系统健康状况进行评价。结果表明:(1)异龙湖流域湿地生态系统健康评价综合分值(Y)为2.8494,处于[2,3]之间,属于脆弱状态;(2)从三大指标状况来看,压力指标(P)、状态指标(S)和响应指标(R)在评价等级中的得分及表现情况分别为0.7368(脆弱状态)、1.1620(亚健康状态)和0.9506(亚健康状态);(3)人口密度、人类活动强度、单位面积化肥和农药负荷、水土流失强度、湖泊水富营养化、人们的环保意识等指标是影响流域内湿地生态系统健康状况的关键因素,人为因素占主导地位。     

新疆和田地区耕地面源污染生态风险评价

随着化肥、农膜等在农业生产中的过量投入,耕地面源污染的程度随之加重。文章选取塔里木河流域上游和田地区为研究区域,依据P-S-R框架理论,构建和田地区耕地面源污染生态风险评价指标体系,加入土壤理化数据,使用生态风险评价模型对和田地区1980 年及2016 年耕地面源污染状况进行生态风险评价,运用耕地生态风险模型、生态风险转移矩阵、Arcgis分析和田地区耕地面源污染时空分异状况。研究结论如下：和田地区1980 年耕地生态风险等级均为II级或III级,呈“中间高,两侧低”分布;2016 年耕地生态风险等级上升至IV级或V级,呈“倒W型”分布,各县耕地面源污染程度较1980 年均有较大幅度的上升,其中墨玉县和于田县在2016 年耕地生态风险等级达到最高的V级,而民丰县因自身生态环境的强脆弱性,同样需要提高关注。根据面源污染“从源头治理”的原则,应切实推进和田地区耕地生态环境保护与治理,提高政府重视程度,增强技术指导,开展试点工作,改善和田地区耕地面源污染现状。     

基于PSR模型的石化园区海洋环境影响后评估指标体系研究

我国将建成七大国家级石化产业园区,这些石化园区无一例外的位于沿海地区或海岛上,为此加强石化园区运营期海洋环境保护意义重大.环境影响后评估是运营期检验园区环境管理水平、查找园区环境问题的重要手段之一.目前,石化园区环境影响后评估主要以环境要素逐一分析法最为常见,而将石化园区作为一个整体从资源、环境、管理等角度综合评估的方法尚不多见.本研究在阐述我国海洋环境后评估和深入分析石化园区用海特点的基础上,结合PSR框架模型加以总结,提出了石化园区海洋环境影响后评估框架与指标体系,分为框架层、方案层和指标层,共25项考核指标,以期为今后沿海石化园区海洋环境管理研究提供思路.同时,本研究明确了各类评估指标赋值和权重等计算方案,并以大连某石化园区为案例进行了评估效果验证.     

基于PSR框架的典型河口富营养化综合评价方法研究

基于PSR(压力-状态-响应)指标框架建立一套适用于我国河口环境的第二代富营养化综合评价体系,该体系的评价指标包括营养物质压力指标、富营养化初级症状指标、富营养化次级症状指标和富营养化其他症状指标四类,并以双台子河口生态监控区为例进行了富营养化综合评价。评价结果表明,2004-2006年间双台子河口生态监控区均未处于富营养的状态,水质质量相对较好。     

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.     

PSR J1012+5307: younger than it looks?

Lorimer et al. have recently reported that the spin-down age (∼7 × 10⁹ yr) of the low-mass binary pulsar PSR J1012+5307 is much higher than the cooling age (3 × 10⁸ yr) of its white dwarf companion. The proposed solutions for this discrepancy are outlined and discussed. In particular, the revised cooling age estimate proposed by Alberts et al. agrees with data from other low-mass binary pulsar systems if a transition to the 'classical' cooling regime occurs between ∼0.14 and ∼0.28 M_⊙. If this transition is excluded, PSR J1012+5307 seems to have finished its accretion phase far from the spin-up line.     

Historical Evidence for the Birth of the Newly Discovered Pulsar PSR J1833-1034

Stimulated by the recent discovery of PSR J1833-1034 in SNR G21.5-0.9 and its age parameters presented by two groups of discovery, we demonstrate that the PSR J1833-1034 was born 2053 years ago from a supernova explosion, the BC 48 guest star observed in the Western Han (Early Han) Dynasty by ancient Chinese. Based on a detailed analysis of the Chinese ancient record of the BC 48 guest star and the new detected physical parameters of PSR J1833-1034, agreements on the visual position, age and distance between PSR J1833-1034 and the BC 48 guest star are obtained. The initial period P0 of PSR J1833-1034 is now derived from its historical and current observed data without any other extra assumption on P0 itself, except that the factor PP is a constant in its evolution until now.