中原城市群与产业群耦合发展研究

依托空间偏离-份额模型建立了产业群与城市群耦合发展的基本分析框架,并对中原城市群进行了定量诊断。研究结果表明:2001—2013年间,首位城市郑州的产业实力和集聚扩散能力显著提升,产业群与城市群的耦合在地理空间呈圈层式扩展态势,然而城市群尚未形成功能等级与分工协作明确的区域综合经济体。继续实施中心城市带动战略、发挥成员城市比较优势促进城际产业链接、完善城市群综合交通运输网络是促进产业群与城市群耦合、提高群域经济发展水平和增强城市竞争力的有效手段。     

农业产业集群的演化阶段与形成机理分析——以宁夏中宁县枸杞加工产业为例

在总结前人研究基础上,借鉴国内外农业产业集群研究的相关理论,以宁夏中宁县枸杞加工产业集群为例,运用企业资料和半结构式访谈法,探讨了农业产业集群的演化阶段和形成机理。研究发现:(1)中宁县枸杞加工产业集群遵循农业产业集群演化的一般发展规律,经历了培育期、成长期及形成期,在不同的发展阶段集群表现出不同特征。(2)地区独特的资源禀赋、历史文化、宏观制度等偶然因素激发集群最初形成,地理临近导致的集聚效应促使集群逐步成长,收益递增引发的路径依赖则进一步促进集群的形成。(3)由于收益递增、路径依赖及企业惯例,集群在演化过程中可能会陷入低效率的锁定状态。为了摆脱这种困境,首先,政府应推动企业间网络合作强度及知识流动,提升集群创新能力;其次,要加强集群与区外联系实现集群在全球价值链上的嵌入,保持集群持续的竞争力。研究结果可为农业产业集群形成及机理研究提供借鉴,为宁夏枸杞加工产业发展提供指导。     

引发强降水的一次东移高原云团的能量演变特征研究

利用日本气象厅葵花-8卫星亮温资料、欧洲中心ERA5（the fifth generation of European Centre for Medium-Range Weather Forecasts Reanalysis）再分析资料,根据时间尺度分解的局地能量诊断方法,本文从能量学多个角度研究了2016年6月5日00时（协调世界时,下同）至6日15时（持续40小时）一次东移并引发强降水的高原对流云团,得到了以下主要结论。本次事件中,高原东移对流云团在不同阶段的主要影响系统有所不同。移出高原前,其主要受高原涡和高原短波槽的共同影响,随着云团移出高原,高原涡消亡,而高原短波槽则随时间发展加强,成为东移云团的最主要影响系统。高原东移对流云团具有显著的深对流特征,自西向东引发了一系列的降水,移出高原后,其对流重心显著降低,降水达到最强。不同阶段高原东移对流云团的能量转换特征显著不同。云团位于高原上时（第一阶段）,背景场通过动能的降尺度能量级串为造成强降水的扰动流直接提供能量,这是此阶段扰动流动能维持的主要方式;云团移出高原过程中（第二阶段）,降水凝结潜热明显增强,由此制造的扰动有效位能也显著增强。在垂直运动配合下,扰动有效位能斜压释放所制造的动能是本阶段造成强降水扰动流动能维持的最主要能量来源;云团移出高原后（第三阶段）,背景场对造成强降水扰动流的影响再次增强,但是不同于第一阶段的直接影响方式,该阶段背景场的作用是以一种间接的影响方式出现。其首先通过有效位能的降尺度级串将背景场的有效位能转换为扰动流的有效位能,然后通过扰动有效位能的斜压能量释放为扰动流的动能维持不断地提供能量。此外,本阶段内还出现了扰动流向背景场动能的升尺度级串供给（即扰动流的反馈）,但其强度不足以对背景场的演变产生显著影响。     

An intercomparison of two rawinsonde systems

Abstract

An intercomparison of the Väisälä MicroCora system used in the Automated Shipboard Aerological Program (ASAP) and the Atmospheric Environment Service upper‐air system (GMD/ADRES) was conducted in May‐June 1983. Thirty‐three paired ascents were made. The ASAP system dry‐bulb temperatures averaged 0.3°C warmer. For the lowest 100 mb, the dew‐point temperature difference (ASAP ‐ GMD/ADRES) was near ‐1°C whereas for the 780–500 mb layer, the difference was 1°C. The wind component mean differences averaged were small but with a 4 m s^?1 standard deviation.     

An Analysis of the Radio Light Variations of Blazars With Low Peak Frequencies

The data of light variations of six blazars with low peak frequencies (i.e., BL Lacerta, 0235+164, OQ530, 0716+714, 3C 345, and 3C 273) at 4.8, 8, 14.5, 22 and 37 GHz in the recent thirty years have been collected from immense amount of literature. By using the method of discrete correlation function the correlations and delays of the light curves of these six sources at the 5 wavebands are analyzed. With the method of structural function, the periods and timescales of the light variations of these six sources are analyzed, and their amplitudes of light variations are compared and analyzed. As revealed by the result of analysis, among the six blazars the amplitudes of light variations of 0716+714 and 0235+164 are relatively large, and those of 3C 345 and OQ 530 are less. The amplitudes of light variations of 3C 273 and BL Lacertae are relatively smaller. As shown by the multi-waveband analysis of delays between two neighboring wavebands, 0235+164 exhibits the tendency of variation that the high-frequency wavebands precede the low-frequency wavebands. On the whole, 3C 345 exhibits the tendency that the high-frequency wavebands lag be-hind the low-frequency wavebands. The analyses of the other blazars show that in a part of radio wavebands there appears the tendency of variation that the high-frequency waveband leads the low-frequency waveband. Yet in the other radio wavebands there appears the tendency that the high-frequency waveband lags behind the low-frequency waveband. As revealed by the results of analyses with the method of structural function, the timescale, fitted slope, and period of light variations of 3C 345 are larger than those of the other five blazars with low peak frequencies. This demonstrates that the activity of 3C 345 is comparatively weaker than the other five sources, and implies that in the interior of 3C 345 there may exist some physical processes which are different from those of the other five blazars with low peak frequencies.     

银河系恒星潮汐流的探测进展

银晕外区存在众多星流,它们或源自银河系的矮伴星系,或源自晕族球状星团,常分别称为矮星系星流和球状星团潮汐尾。星流可以利用各类示踪星,并通过不同的途径加以探测,对若干代表性矮星系星流和球状星团潮汐尾的探测进展做了简要的介绍。     

基于聚合点的网络多媒体业务拥塞控制

当前广泛开展的网络多媒体业务都存在不同程度的服务不稳定情况,其原因是架构于网络上的多媒体业务缺乏整体有效的网络控制机制.基于研究提出了一种基于聚合点的拥塞控制方法,能对网络多媒体业务进行有效的拥塞控制.与现有业务实施机制相比,该方案实现简单,能更有效保证业务的开展.     

星爆后星系NGC4736核区的环状结构

在１９９２年３月３１日至４月２日期间，我们利用云南天文台１ｍ望远镜２号ＣＣＤ和缩焦装置，对环星系ＮＧＣ４７３６进行了Ⅴ和Ⅰ波段深曝光观测。在经过Ｒｉｃｈａｒｄｓｏｎ－Ｌｕｃｙ图象复原以及自适应滤波两种方法处理后，发现仅仅在Ⅴ波段图象上，其核区存在一个直径约为１０″的环状结构。     

Numerical simulations of the Hyades dynamics and the nature of the moving Hyades cluster

We present our numerical simulations of the dynamical evolution of the Hyades open cluster. The simulations were performed usinga modified NBODY6 algorithm that included tidal forces and a realistic orbit of the cluster in a gravitational field described by the Miyamoto-Nagai potential. Our goal was to study the nature of movingclu sters. We show that the stars that were earlier cluster members could be later identified within a sphere of 50 pc in diameter around the Sun. The number of such stars for the chosen initial mass and virial radius of the cluster does not exceed ten. The maximum space velocity of these stars relative to the core of the current cluster does not exceed 3 km s^?1. Our numerical simulations confirm the assumption that some of the moving clusters near the Sun could consist of stars that have escaped from open clusters in the course of their dynamical evolution.     

NGC 1624 (OCl 403, Cr 53) – A very young open cluster

We present the first CCD photometric UBVRI observations of the not-so-well-studied open cluster NGC 1624 (OCl 403, Cr 53; α₂₀₀₀ = 04 h 40 m 36 s; δ₂₀₀₀ = + 50^˚ 27^′ 42″ Trumpler class = I 2 p N). This cluster was observed on 01 February 2004 with the 2 m Himalayan Chandra Telescope at Hanle using a LN2 cooled 2k × 2k CCD. The cluster presents differential reddening with E(B-V) values ranging from 0.70 to 0.90 mag, which could be attributed to the presence of the HII region wherein the cluster is embedded. It is found to be at a distance of 6.025 ± 0.5 kpc and the age of this cluster is estimated to be ∼3.98 × 10⁶ years. In view of these parameters, it can be considered as a young enough cluster located in the direction of the Perseus constellation with the galactic coordinates of l = 155^˚.35 and b = + 02 ^˚.58. Thus it could also be used as a suitable candidate for tracing the Outer Perseus spiral arm of our Galaxy. The initial mass function slope is derived as 1.65 ± 0.25 by applying the corrections for field star contamination and data incompleteness. This is in good agreement with the Salpeter value within the limits of errors.