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.     

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.     

基于DBBC＋Mark5B记录系统的脉冲星观测

2009年11月,云南天文台射电天文研究团组采用40m射电望远镜以及基于DBBC（Digital Base Band Conveter）和Mark5B的VLBI记录系统对PSRJ08354510和PSRJ0332＋5434进行了观测。观测选用S波段右旋圆极化信号,起始频率为2206．99MHz,总带宽为32MHz。对数据进行相干消色散和平均后,得到PSRJ0332＋5434的单脉冲图像和两颗脉冲星的平均脉冲轮廓。由平均轮廓的展宽随时间的变化关系,对脉冲星的视周期作了一定修正后,得到信噪比更高的平均轮廓图。最后对轮廓的信噪比随时间的变化作了初步分析,由此可了解整个系统在观测时的稳定性。     

基于PSR 模型的厦门湾中华白海豚资源评价

中华白海豚(Sousa chinensis Osbeck,1765)为国家Ⅰ级重点野生保护动物,厦门湾作为其在中国的主要分布区之一,自20世纪80年代以来,海岸带开发活动和环境污染程度均不断加大,导致此海域中华白海豚的生存环境不断恶化,种群数量日趋减少,资源状况面临严重威胁。作者采用PSR(压力-状态-响应)模型框架,对厦门湾中华白海豚资源面临的主要环境压力、当前的资源状态以及采取的保护响应措施进行了一个较全面的评价,评价结果认为:围填海工程、船只交通、水下爆破作业和陆源排污等人类活动给厦门湾中华白海豚带来了生境缩小、身体伤害、环境污染和饵料短缺等严重影响,厦门市已采取的保护政策响应包括就地保护、迁地保护和公共管理等方面,目前种群资源数量稳定在80头左右并有潜力扩大。基于评价结果,作者提出了加强保护的建议和策略,可为厦门以外海区的中华白海豚保护工作提供参考。