从珠三角到大珠三角再到粤港澳大湾区：改革开放以来中国的国家尺度重组

尺度重组是解释当前国家、城市等地域组织参与全球化竞争的工具媒介。文章以中国华南地区改革开放以来广东、香港、澳门三地跨界合作为例,借鉴行动者网络理论的研究方法深入剖析珠三角、大珠三角及粤港澳大湾区3个“新国家空间”的尺度重组过程,揭示中国尺度重组的政治经济逻辑。研究发现,行动者拥有的资源决定了其在尺度网络中的地位,而中国的“新国家空间”形成主要依托中央政府推动,其发展目标的设定具有决定性作用,港澳特区政府、广东省地方政府、乡镇企业和外资企业等其他行动者在协同合作中将自身的发展目标与之融合形成了“强制通过点”。纵观三阶段的演变过程,制度因素的重要性越来越得到凸显。     

Interactive Effects of Ultraviolet Radiation and Dissolved Organic Carbon on Phytoplankton Growth and Photosynthesis in Sanya Bay,Northern South China Sea

Ocean Science Journal - The effects of a simulated climate change scenario, i.e., increased ultraviolet radiation (UVR) and dissolved organic carbon (DOC), on the growth and photosynthesis of...     

解郁降压颗粒结合音乐疗法对围绝经期高血压病大鼠性激素水平的影响

目的：观察解郁降压颗粒结合音乐疗法对围绝经期高血压病模型大鼠性激素的调节作用,初步探讨解郁降压颗粒结合音乐疗法治疗围绝经期高血压病的可能机制。方法：选用动情周期规律的SPF级雌性自发性高血压（SHR）大鼠,将其随机分成SHR组、假手术组、围绝经期高血压病模型组（简称模型组）、解郁降压颗粒加音乐疗法组（简称治疗组）;另设WKY大鼠作为正常血压对照组。通过摘除双侧卵巢方法建立围绝经期高血压病模型,待造模成功后,予以相应干预。治疗结束后测量血清雌二醇（E_{2）、促卵泡生成素（FSH）、促黄体生成素（LH）的含量,同时测量大鼠动脉血管的平均光密度值（OD值）。结果：与SHR组比较,治疗组血压下降,差异有统计学意义（P<0.05）;与模型组比较,治疗组E22上升,OD值上升,FSH、LH含量下降,差异均有统计学意义（P<0.05）。结论：解郁降压颗粒结合音乐疗法对围绝经期高血压病模型大鼠有降压作用,且能提高SHR模型大鼠血清E22的含量,降低FSH、LH含量,改善SHR模型大鼠的内分泌环境;OD值上升,表示雌激素α受体（ERα）水平提高;而对内分泌环境的改善和ERα水平的提高可能是其降压机制之一。}     

耀变体在射电波段的偏振研究

利用UMRAO数据库22个耀变体源的偏振数据,根据Lazarian&Pogosyan理论模型分析研究了耀变体射电波段的偏振随波长的变化,得出不同类的耀变体偏振随波长变化的原因。结果表明,与Lazarian&Pogosyan理论模型吻合较好。由此得出如下结论:(1)反常去偏振耀变体源中反常法拉第旋光起主导作用,反常去偏振相对较少;(2)热辐射与同步辐射混合作用,高频波段的偏振度小于低频波段的偏振度(反常去偏振);(3)当被观测波段波长小于吸积盘热辐射对应的维恩波长时,高频波段的偏振度大于低频波段的偏振度(常规去偏振)。     

南山26米射电望远镜轨道高差测量及其对指向精度的影响

轮轨式天线的轨道作为承载整个天线重量的基础,其精度直接影响天线在方位方向运转的平稳性,引起天线轴系偏差从而影响天线的指向精度。介绍改造后的乌鲁木齐南山26 m射电望远镜(Nanshan Radio Telescope, NSRT)轨道结构以及轨道高差测量,并建立天线在不同方位、俯仰角下轨道高差引起天线指向偏差的数学模型。利用"十字扫描"法实测多颗标准源在相应位置的指向数据,并通过高斯拟合得到指向偏差。通过分析可知,轨道高差引起的指向偏差经过修正可以提高天线的指向精度。     

天文CMOS相机测试平台及控制系统的实现

CMOS相机是一种重要的固体成像设备?随着科研级CMOS相机的性能不断提高,现已广泛应用于科研领域?新真空太阳望远镜的成像设备也使用CMOS相机?因此建立一个天文CMOS相机测试系统?对于新购CMOS相机的验收以及现有CMOS相机的定期检测和维护有十分重要的意义。介绍了CMOS相机测试平台的硬件组成,并针对实际测试中对设备控制的需求,以及利用控制器对相应的设备直接控制,提出了基于TCP/IP协议以及串口通信的设计方案?利用C#编程语言设计了一套多线程并行的控制系统软件?实现各设备在局域网内的远程并行控制。通过对设备的运行测试,结果表明,系统能良好地控制各设备的正常运行?满足测试系统集成控制的需求.     

球面距离计算方法及精度比较

球面距离(角间距)计算是天文或地理学中极常用的计算之一,也是目标查找、锥形检索、交叉证认等方法的基础。数学上,通过球面几何可以直接计算出两点的距离,前人已经推导出了多个复杂程度不一的计算方法。但是由于计算机的精度有限,在进行数值计算时有舍入误差,导致公式计算结果出现偏差。对几个常用的球面距离计算公式进行了考察,测试并对比它们在不同计算环境下的精度与优缺点。此外还展示并比较了几种常用天文软件包、数据库的球面距离计算方法,以期有助于天文工作者选择适合自己当前需要的计算方法。     

Orbital evolution of a planet with tidal dissipation in a restricted three-body system

The angle between planetary spin and the normal direction of an orbital plane is supposed to reveal a range of information about the associated planetary formation and evolution. Since the orbit's eccentricity and inclination oscillate periodically in a hierarchical triple body and tidal friction makes the spin parallel to the normal orientation of the orbital plane with a short timescale in an isolated binary system, we focus on the comprehensive effect of third body perturbation and tidal mechanism on the angle. Firstly, we extend the Hut tidal model(1981) to the general spatial case, adopting the equilibrium tide and weak friction hypothesis with constant delay time, which is suitable for arbitrary eccentricity and any angle ? between the planetary spin and normal orientation of the orbital plane. Furthermore, under the constraint of angular momentum conservation, the equations of orbital and ratational motion are given. Secondly, considering the coupled effects of tidal dissipation and third body perturbation, and adopting the quadrupole approximation as the third body perturbation effect, a comprehensive model is established by this work. Finally, we find that the ultimate evolution depends on the timescales of the third body and tidal friction. When the timescale of the third body is much shorter than that of tidal friction, the angle ? will oscillate for a long time,even over the whole evolution; when the timescale of the third body is observably larger than that of the tidal friction, the system may enter stable states, with the angle ? decaying to zero ultimately, and some cases may have a stable inclination beyond the critical value of Lidov-Kozai resonance. In addition, these dynamical evolutions depend on the initial values of the orbital elements and may aid in understanding the characteristics of the orbits of exoplanets.     

The galaxy luminosity function in the LAMOST Complete Spectroscopic Survey of Pointing Area at the Southern Galactic Cap

We present optical luminosity functions(LFs) of galaxies in the~(0.1) g,~(0.1) r,~(0.1) i bands, calculated using data in~40 deg~2 sky area of the LAMOST Complete Spectroscopic Survey of Pointing Area(LaCoSSPAr) in the Southern Galactic Cap. Redshifts for galaxies brighter than r = 18.1 were obtained mainly with LAMOST. In each band, LFs derived using both parametric and non-parametric maximum likelihood methods agree well with each other. In the0.1 r band, our fitting parameters of the Schechter function are φ_*=(1.65 ± 0.36) × 10~(-2) h~3 Mpc~(-3), M_*=-20.69 ± 0.06 mag and α =-1.12 ± 0.08,which agree with previous studies. Separate LFs are also derived for emission line galaxies and absorption line galaxies. The LFs of absorption line galaxies show a dip at~(0.1) r ~18.5 and can be fitted well by a double-Gaussian function, suggesting a bimodality in passive galaxies.