构建“三强三化”保障体系 推进数字化档案建设取得实效

在城市规模不断扩张的当下,自然资源档案的数据量飞速增长,内容日趋多元,传统模式下的档案管理手段方法已较难满足时代发展需求。为此,杭州市规划和自然资源局江干分局紧紧围绕职能机构改革这一重要契机,全面推进档案信息化建设迭代升级,以数字化转型为引领,不断构建制度规范化、采编智能化、运用便利化的服务体系。近年来,该局通过不懈努力,在业务档案方面实现了100%数字化覆盖,连续十一年档案年检考核优秀,2021年被浙江省档案局评选为“示范数字档案室”。     

嫦娥五号荷“月”而归

2020年11月24日凌晨4时30分,长征五号火箭将嫦娥五号月球探测器送出地球;2020年12月17日1时59分,嫦娥五号返回器携带着从月球挖到的月壤,安全回到祖国大地。23天的探月之旅,嫦娥五号完成了一次对接、六次分离,两种方式采样、五次样品转移,经历了11个重大阶段和关键步骤,满载而归。     

用日全食光谱探测太阳中低层大气对局部热动平衡的偏离

在太阳大气不同层次连续光谱中叠加有丰富的发射线或吸收线,对这些谱线轮廓进行反演分析可以探测太阳大气的化学成分和物理状态.太阳大气的色球及过渡区由于其密度低难以建立热动平衡,建立相应的大气模型需要采用非局部热动平衡(Non-Local Thermodynamic Equilibrium,N-LTE)理论.根据相对偏离因子计算来研究太阳中低层大气偏离局部热动平衡(Local Thermodynamic Equilibrium,LTE)分布的情况.首先对日全食观测过程中得到色球和过渡区不同高度形成的两条光谱数据进行反演,得到确定观测谱线的参数信息,如连续谱源函数、谱线源函数、多普勒宽度和由此推出的等效动力学温度;根据这些反演出的谱线参量计算出二维视场内每个空间采样点偏离LTE状态的定量结果;其次,根据用于观测的积分视场单元光纤排布阵列重构出辐射强度、等效动力学温度和相对偏离因子二维分布.结果显示:在局部小区域,温度分布和相对偏离因子的分布存在较强相关性,而与辐射强度分布无明显相关.从两条谱线导出的等效温度和相对偏离因子分布存在明显的差异.这两种二维分布揭示出太阳大气某些小尺度区域具有较强的结构性和复杂性,为进一步理解太阳中低层大气物理提供了一种新的视角.     

基于NPSVM模型的超新星识别方法

巡天观测与高能物理、黑洞天文等领域均有密切的联系.基于星系-超新星二分类问题,研究光谱数据预处理,结合余弦相似度改善PCA(Principal Component Analysis)光谱分解特征提取方法,用SDSS(the Sloan Digital Sky Survey)、WISeREP(the Weizmann Interactive Supernova data REPository)组成的5620条光谱数据集训练支持向量机,可以得到0.498%泛化误差的识别模型和新样本分类概率.使用Neyman-Pearson决策方法建立NPSVM(Neyman-Pearson Support Vector Machine)模型可进一步降低超新星的漏判率.     

基于双谱滤波的综合脉冲星时算法研究

毫秒脉冲星的自转频率非常稳定,提供了一种独立的基于遥远自然天体并能持续数百万乃至数十亿年的时间基准,具有稳定性强、运行时间长、服务范围广等特点.为了减弱毫秒脉冲星计时观测中各种高斯噪声对脉冲星时的影响,研究了一种基于双谱滤波的综合脉冲星时构建算法,处理分析了国际脉冲星计时阵(International Pul-sar Timing Array,IPTA)最新发布的4颗毫秒脉冲星(PSR J0437-4715、J0613-0200、J1713+0747和J1909-3744)的观测数据,分析了不同时间尺度综合脉冲星时的稳定性,并与构成国际原子时(International Atomic Time,TAI)的4家授时单位原子钟稳定性进行了比较.结果表明:双谱滤波算法能够较好地抑制观测噪声,提高综合脉冲星时的稳定性.相比于经典加权算法,综合脉冲星时1 yr、10 yr稳定度从7.77×10^-14、8.56×10^-16分别提高到1.50×10^-14、3.50×10^-16,单脉冲星时稳定性的提升也类似.同时发现,综合脉冲星时稳定性在5 yr及以上时间尺度上优于原子钟稳定性,可用于改善当前原子时的长期稳定性.     

走近空间医学

小时候,我想当一名宇航员。我梦想着飞向月球。现在,我成了一名天文学家,但是对载人航天一直保持着兴趣。成为宇航员的梦想很好,但是对真正飞向太空进行一番思考,你就会意识到,当宇航员比你能想到的还要危险。空间站发生空气泄漏怎么办?你每天吃什么?如果你在长途国际航班上都感到无聊,那么坐在-艘小小的飞船里,花六个月的时间飞往火星,这样的旅途又将是怎样的感受!如果你和飞船里其他的队员起了冲突怎么办?如果你感冒了,或者牙疼,或者得了癌症,又该怎么办?人的身体最适合在地球表面、与其他人一起生活。人的身体和精神所能应付的事是有限的,这就是为什么,我们向太阳系内各行星发射的大多是自动探测器。不过,在不久的将来,我们必须学会如何解决这些问题。     

下辽河平原景观格局演变与预测分析

以下辽河平原为研究对象,选取1980年、2010年和2018年Landsat TM/ETM+OLI卫星图像进行解译,得到3期土地利用数据,定量分析下辽河平原近40年土地利用时空变化特征.结合地形、交通通达度及限制转化因子采用FLUS(Future Land Use Simulation)模型对流域未来土地利用变化情景及景观格局进行了预测.结果表明:1980-2018年水田、林地、草地、沼泽面积均减少,其中水田面积减少量最大,占比减少了8.59％,旱地、水域和城镇的面积均有所上升,旱地的增长面积最大,占比增加了6.19％;水田、林地、水域转入为旱地面积最大,旱地转出为建设用地面积最大;1980-2018年景观格局发生了较大变化,景观的破碎化程度降低,斑块之间的连通度、聚集程度升高,土地利用的集约化程度增大;2018-2040年,下辽河平原建设用地和水田的变化面积最大,城市化过程更加显著,景观的多样性及空间异质性降低,人类对环境的干扰能力变大.     

The conformity of HI galaxies in ALFALFA-SDSS sample

The conformity effect,indicating the evolution of galaxies is related to its surrounding neighbor galaxies as far as a few Mpc,is an interesting phenomenon in the modeling of galaxy and evolution.Here we study the conformity effect of HI galaxies in a matched galaxy sample between SDSS DR7 and ALFALFA surveys.By checking the probability difference for the detected H i galaxies as a function of distance around a normal or an H i galaxy,we find that this effect is significant out to 5 Mpc.It also shows a dependence on the stellar mass of galaxies,with the strength the strongest in the stellar mass range of 10¹⁰*/M_⊙<10^10.5.However,when the sample is confined to central galaxies in groups with virial radii smaller than 1 Mpc,the 1-halo conformity signal is still evident,while the 2-halo conformity signal is reduced to a very weak amplitude.Our results confirm the previous study in the optical band that the 2-halo term is possibly caused by the bias effect in the sample selection.Furthermore,we confirm the existence of the 1-halo conformity discovered in the optical and radio band in previous investigations.Our results provide another viewpoint on the conformity effect and hope to shed light on the co-evolution of the galaxies and their neighbors in the current galaxy formation models.     

The electromagnetic and gravitational-wave radiations of X-ray transient CDF-S XT2

Binary neutron star(NS)mergers may result in remnants of supra-massive or even stable NS,which have been supported indirectly by observed X-ray plateau of some gamma-ray burst(GRB)afterglows.Recently,Xue et al.(2019)discovered an X-ray transient CDF-S XT2 that is powered by a magnetar from merger of double NS via X-ray plateau and following stepper phase.However,the decay slope after the plateau emission is slightly larger than the theoretical value of spin-down in electromagnetic(EM)dominated by losing its rotation energy.In this paper,we assume that the feature of X-ray emission is caused by a supra-massive magnetar central engine for surviving thousands of seconds to collapse into a black hole.Within this scenario,we present the comparisons of the X-ray plateau luminosity,break time,and the parameters of magnetar between CDF-S XT2 and other short GRBs with internal plateau samples.By adopting the collapse time to constrain the equation of state(EOS),we find that three EOSs(GM1,DD2,and DDME2)are consistent with the observational data.On the other hand,if the most released rotation energy of magnetar is dominated by GW radiation,we also constrain the upper limit of ellipticity of NS for given EOS,and its range is[0.32-1.3]×10^-3.Its GW signal cannot be detected by Advanced LIGO or even for more sensitive Einstein Telescope in the future.     

GRB 130310A: very high peak energy and thermal emission

The special GRB 130310 A was observed by Fermi Gamma-Ray Burst Monitor and Large Area Telescope,with T90~2.4 s.With a combination of a Band function and a blackbody(BB)function,the time-resolved spectral analysis of GRB 130310 A confirmed that there is a sub-dominate thermal component in the early period(e.g.,slice T0+[4.03-4.14]s)spectrum with BB temperature(kT)being~7~5 keV,which can be interpreted as photosphere emission.The precursor of GRB 130310 A can be fitted well with a BB component with kT~45 keV,which is higher than that of the main burst.It suggests that the radiation of GRB 130310 A is in transition from thermal to non-thermal.Such a transition is an indication of the change in jet composition from a fireball to a Poynting-flux-dominated jet.A very high peak energy is obtained in the first time bin,with the peak energy E_p of the Band component for Band+BB and Band model being~8.5~5.2 MeV and~11.1~7.4 MeV,respectively.Afterwards,the E_p drops to~1 MeV.The E_p evolution patterns with respect to the pulses in the GRB 130310 A light curves show a hard-to-soft evolution.The interpretation of the high peak energy E_p within the photosphere and internal shock model is difficult.It also suggests that at least for some bursts,the Band component must invoke a non-thermal origin in the optically thin region of a GRB outflow.Assuming the redshift is z~0.1~8,the radius of the jet base r₀~10⁹ cm to allow(1+σ₁₅)>1 in line with the calculation results of the magnetization parameter at~1015 cm(σ₁₅).However,the value of(1+σ₁₅)is■1 in the zone z around 3 for r₀~10⁹ cm,suggesting the non-excluded possibility that the origin is from ICMART with a low value.The photosphere-internal shock seems capable of interpreting the high peak energy,which requires electron Lorentz factorγe~60 andεe~0.06.