Pulsar slow glitches in a solid quark star model

A series of five unusual slow glitches of the radio pulsar B1822–09 (PSR J1825–0935) was observed between 1995 and 2005. This is a phenomenon that is understood in a solid quark star model, and reasonable parameters for slow glitches are given in this paper. We propose that, because of increasing shear stress as the pulsar spins down, a slow glitch may occur, beginning with the collapse of a superficial layer of the quark star. This layer of material turns to viscous fluid at first, the viscosity of which helps to deplete the energy released from both the accumulated elastic energy and the gravitation potential. There is then a slow glitch. Numerical calculations show that the slow glitches that have been observed could be reproduced if the effective coefficient of viscosity is ∼10² cm² s⁻¹ and the initial velocity of the superficial layer is of the order of 10⁻¹⁰ cm s⁻¹ in the coordinate rotating frame of the star.     

Open clusters IC 4665 and Cr 359 and a probable birthplace of the pulsar PSR B1929+10

Based on the epicyclic approximation, we have simulated the motion of the young open star clusters IC 4665 and Collinder 359. The separation between the cluster centers is shown to have been minimal 7 Myr ago, 36 pc. We have established a close evolutionary connection between IC 4665 and the Scorpius-Centaurus association — the separation between the centers of these structures was ≈200 pc 15 Myr ago. In addition, the center of IC 4665 at this time was near two well-known regions of coronal gas: the Local Bubble and the North Polar Spur. The star HIP 86768 is shown to be one of the candidates for a binary (in the past) with the pulsar PSR B1929+10. At the model radial velocity of the pulsar V _r = 2 ± 50 km s^?1, a close encounter of this pair occurs in the vicinity of IC 4665 at a time of ?1.1 Myr. At the same time, using currently available data for the pulsar B1929+10 at its model radial velocity V _r = 200 ± 50 km s^?1, we show that the hypothesis of Hoogerwerf et al. (2001) about the breakup of the ζ Oph-B1929+10 binary in the vicinity of Upper Scorpius (US) about 0.9 Myr ago is more plausible.     

利用南山数据对PSR B0329+54的长时标轮廓稳定性的研究

利用新疆天文台25 m射电望远镜2003—2009年对PSR B0329+54长达453 h的观测数据,研究了这颗源在1540 MHz上正常模式和反常模式的轮廓稳定性时标.通过不同时间的积分脉冲轮廓与参考轮廓交叉相关系数分析,发现随积分时间的增加,两种模式的轮廓先是以较快的速度趋于稳定,在积分时间增加到约(4±1) min时,轮廓趋稳速率放缓,当积分时间达到(140±60) min (正常模式)或达到(65±15) min (反常模式)时,轮廓趋稳速度再次变快.相关系数的结果显示两种模式的轮廓在绝大多数积分时标上都不是完全随机的涨落.如果以发生轮廓趋稳速率从快到慢转变所需的积分时间作为轮廓稳定时标的判据,两种模式的稳定时标均大约为5 min.轮廓中不同成分强度比例的涨落随积分时间的变化关系各不相同,由此可以推断3个成分强度涨落性质有差异.造成轮廓趋稳行为在不同时标上有明显差异的原因有观测噪声和星际闪烁等.     

东太湖水生植物及其与环境的相互作用

通过PSR模型建立福建山仔水库生态安全评价的指标体系,应用熵权法确定各指标权重,引入密切值法对水库的生态安全进行评价．结果表明,2000—2003年福州市山仔水库生态安全状况从优到劣的排序依次为：2002年、2001年、2000年、2003年．该研究改进了水库生态安全评价指标体系和传统生态安全评价的数学模型,使指标体系更合理、更切合水库的生态环境保护目标,计算简便,能较客观、全面地反映出评价对象各样本状况．     

基于PSR模型的胶州湾生态安全评价研究

科学有效地评价胶州湾生态安全程度,是胶州湾地区可持续发展的前提。文章基于PSR模型建立评价指标体系,利用AHP-熵权法确立指标权重,对2007—2016年胶州湾生态安全的发展状况进行了综合评价,并从压力、状态、响应3个方面对影响胶州湾生态安全的主要因素进行系统分析。研究结果表明:胶州湾生态安全指数整体呈波动上升态势,但在2010—2013年略有下降,并在2014年有大幅度的回升直至2016年。生态安全指数在0.4～0.6间波动,整体处于"一般"的生态安全状态。最后,文章提出通过坚持控制入海污水排放量和环境污染,加强海洋生态保护修复与海洋保护区建设,进一步完善胶州湾生态安全保护相关法律制度,注重海洋科技人才培养等方式来促进胶州湾地区生态安全水平的提高。     

Cooling curves and initial models for low-mass white dwarfs (<0.25 M⊙) with helium cores

We present a detailed calculation of the evolution of low-mass (<0.25 M_⊙) helium white dwarfs. These white dwarfs (the optical companions to binary millisecond pulsars) are formed via long-term, low-mass binary evolution. After detachment from the Roche lobe, the hot helium cores have a rather thick hydrogen layer with mass between 0.01 and 0.06 M_⊙. As a result of mixing between the core and outer envelope, the surface hydrogen content ( X _surf) is 0.5–0.35 , depending on the initial value of the heavy element Z and the initial secondary mass. We found that the majority of our computed models experience one or two hydrogen shell flashes. We found that the mass of the helium dwarf in which the hydrogen shell flash occurs depends on the chemical composition. The minimum helium white dwarf mass in which a hydrogen flash takes place is 0.213 M_⊙ ( Z =0.003), 0.198 M_⊙ ( Z =0.01), 0.192 M_⊙ ( Z =0.02) or 0.183 M_⊙ ( Z =0.03). The duration of the flashes (independent of chemical composition) is between a few ×10⁶ and a few ×10⁷ yr. In several flashes the white dwarf radius will increase so much that it forces the model to fill its Roche lobe again. Our calculations show that the cooling history of the helium white dwarf depends dramatically on the thickness of the hydrogen layer. We show that the transition from a cooling white dwarf with a temporarily stable hydrogen-burning shell to a cooling white dwarf in which almost all residual hydrogen is lost in a few thermal flashes (via Roche lobe overflow) occurs between 0.183 and 0.213 M_⊙ (depending on the heavy element value).     

基于PSR框架的内蒙古自治区沙漠化敏感性评估

沙漠化敏感性是测度区域沙漠化可能性的关键指标。鉴于沙漠化敏感性研究“重评价、缺框架”、“重格局、轻变化”的研究现状,本文基于“压力—状态—响应”(Pressure-State-Response, PSR)分析框架,构建了“气候条件—地表覆盖—植被恢复”沙漠化敏感性综合评价指标体系,定量评估了2000、2015年内蒙古自治区(除流动沙地(丘)外)沙漠化敏感性,结合县域人口密度开展了区域沙漠化防治分区。研究结果表明：2015年研究区以中度敏感区为主(27.04%),其次为轻度敏感区(25.53%)、不敏感区(22.96%)和高度敏感区(20.82%),极敏感区占比最小(3.65%),沙漠化敏感性呈现出中西部高、东部低的空间格局;2000-2015年间,内蒙古自治区9.20%的土地沙漠化敏感性等级降低,24.83%则趋于增强。研究区可划分为生态保育区、沙化治理区、综合发展区和生态移民区四大沙漠化防治区。     

基于PSR框架模型的南四湖健康评价

根据＂压力-状态-响应＂（PSR）框架模型,对南四湖健康状态进行评价。选取南四湖流域人口密度、工农业供水需求、富营养化程度、南四湖生物多样性指数、环保投资指数等能够充分反映南四湖压力、状态和响应的指标构建评价指标体系;通过专家经验赋值法对各评价指标进行权重确定,并对指标进行标准化赋值;提出了南四湖健康评价模型并且得出南四湖的健康综合指数;根据健康综合指数,确定南四湖健康状况。研究结果表明,南四湖健康评价指数为0.4051,南四湖健康处于＂亚健康＂状态。     

基于PSR-熵权综合健康指数法的城市湖泊生态系统健康评价

本文结合城市湖泊生态系统的特点,利用OECD(联合国经济合作开发署)建立的压力-状态-响应(PSR)框架模型建立指标体系,将信息熵(IE)理论引入指标权重的确定,建立了城市湖泊生态系统健康评价模型,选用综合健康指数法(CHIM)进行城市湖泊生态系统健康评价,并应用山东省聊城市东昌湖的实测资料,对其生态系统健康状况进行了评价,评价结果与实际情况基本相符.     

Determination of the orbital parameters of binary pulsars

We present a simple method for determination of the orbital parameters of binary pulsars, using data on the pulsar period at multiple observing epochs. This method uses the circular nature of the velocity space orbit of Keplerian motion and produces preliminary values based on two one-dimensional searches. Preliminary orbital parameter values are then refined using a computationally efficient linear least-squares fit. This method works for random and sparse sampling of the binary orbit. We demonstrate the technique on (i) the highly eccentric binary pulsar PSR J0514−4002 (the first known pulsar in the globular cluster NGC 1851) and (ii) 47 Tuc T, a binary pulsar with a nearly circular orbit.