基于"PSR+RS"模式的菩提岛整治修复前后生态系统健康评价

海岛生态系统是海洋生态系统的重要组成部分。近年来,随着海岛人为活动数量不断增加,加速了对海岛生态环境的破坏,一些海岛生态失衡严重,生态系统受损加剧。而对受损海岛生态系统开展人工参与下的主动式生态恢复,是目前较为主流的恢复方法和手段,菩提岛整治修复项目正是基于上述修复理念开展并完成的。本文以菩提岛海岛及周边海域为研究区域,基于PSR模型,以RS方式为主要指标获取方式,构建了适用于我国海岛整治修复模式下的海岛生态系统健康评价体系,对其整治修复前后生态系统健康状况开展评价分析。结果显示:2008年,该岛生态系统健康值IEI为0.374 0,生态系统较脆弱,整体状况较差,亟须开展保护与修复工作;2014年,经岛体修复并趋于稳定状态后,该岛生态系统健康值IEI提升至0.673 8,生态系统较健康,处于稳定状态,但仍具有上升空间。经整治修复前后纵向对比,生态系统健康波动值ΔIEI为0.299 8,表明该岛生态系统经过修复后已有所好转。     

深圳湾福田红树林保护区生态系统健康评价

基于PSR模型建立了深圳湾福田红树林保护区生态系统健康评价体系,运用层次分析法对保护区健康状况进行评价。结果表明:保护区生态系统的压力、状态、响应在体系中的比例分别为53.89%、29.73%、16.38%,健康指数分别为0.4080、0.5891、0.6037;保护区综合健康指数为0.4939,处于健康等级Ⅲ级(亚健康状态)。造成以上结果的主要原因为:1近30年来城市化发展导致保护区生态系统丧失部分生态功能,健康水平不断下降;2水污染、人工引种植物和病虫害等对保护区造成巨大外界压力;3建筑施工和人类活动影响保护区自然状态的恢复。     

An empirical model for the polarization of pulsar radio emission

We present an empirical model for single pulses of radio emission from pulsars based on Gaussian probability distributions for relevant variables. The radiation at a specific pulse phase is represented as the superposition of radiation in two (approximately) orthogonally polarized modes (OPMs) from one or more subsources in the emission region of the pulsar. For each subsource, the polarization states are drawn randomly from statistical distributions, with the mean and the variance on the Poincaré sphere as free parameters. The intensity of one OPM is chosen from a lognormal distribution, and the intensity of the other OPM is assumed to be partially correlated, with the degree of correlation also chosen from a Gaussian distribution. The model is used to construct simulated data described in the same format as real data: distributions of the polarization of pulses on the Poincaré sphere and histograms of the intensity and other parameters. We concentrate on the interpretation of data for specific phases of PSR B0329+54 for which the OPMs are not orthogonal, with one well defined and the other spread out around an annulus on the Poincaré sphere at some phases. The results support the assumption that the radiation emerges in two OPMs with closely correlated intensities, and that in a statistical fraction of pulses one OPM is invisible.     

PSR J1453+1902 and the radio luminosities of solitary versus binary millisecond pulsars

We present 3 yr of timing observations for PSR J1453+1902, a 5.79-ms pulsar discovered during a 430-MHz drift-scan survey with the Arecibo telescope. Our observations show that PSR J1453+1902 is solitary and has a proper motion of  8 ±  2  mas yr⁻¹. At the nominal distance of 1.2 kpc estimated from the pulsar's dispersion measure, this corresponds to a transverse speed of  46 ± 11   km s⁻¹  , typical of the millisecond pulsar population. We analyse the current sample of 55 millisecond pulsars in the Galactic disc and revisit the question of whether the luminosities of isolated millisecond pulsars are different from their binary counterparts. We demonstrate that the apparent differences in the luminosity distributions seen in samples selected from 430-MHz surveys can be explained by small-number statistics and observational selection biases. An examination of the sample from 1400-MHz surveys shows no differences in the distributions. The simplest conclusion from the current data is that the spin, kinematic, spatial and luminosity distributions of isolated and binary millisecond pulsars are consistent with a single homogeneous population.     

Spatially resolved STIS spectra of the gravitationally lensed broad absorption line quasar APM08279+5255: the nature of component C and evidence for microlensing

PSR J1806−2125 is a pulsar discovered in the Parkes multibeam pulsar survey with a rotational period of 0.4 s and a characteristic age of 65 kyr. Between MJDs 51462 and 51894 this pulsar underwent an increase in rotational frequency of  Δ ν / ν ≈16×10^-6  . The magnitude of this glitch is ∼2.5 times greater than any previously observed in any pulsar and 16 times greater than the mean glitch size. This Letter gives the parameters of the glitch and compares its properties with those of previously observed events. The existence of such large and rare glitches offers new hope for attempts to observe thermal X-ray emission from the internal heat released following a glitch, and suggests that pulsars which previously have not been observed to glitch may do so on long time-scales .     

Toward an Understanding of the Periastron Puzzle of PSR B1259-63

Efforts are made to understand the timing behaviors (e.g., the jumps in the projected pulsar semimajor axis at the periastron passages) observed in the 13-year monitoring of PSR B1259-63. Planet-like objects are suggested to orbit around the Be star, which may gravitationally perturb the (probably low mass) pulsar when it passes through periastron. An accretion disk should exist outside the pulsar's light cylinder, which creates a spindown torque on the pulsar due to the propeller effect. The observed negative braking index and the discrepant timing residuals close to periastron could be related to the existence of a disk with a varying accretion rate. A speculation is presented that the accretion rate may increase on a long timescale in order to explain the negative braking index.