粤西沿海“4.20”特大暴雨特征分析

根据气象常规观测资料、湛江新一代天气雷达资料、CFL-08风廓线雷达资料及卫星云图,分析2012年4月20日粤西沿海特大暴雨的天气环流形势、能量场、对流不稳定度、水汽输送和辐合辐散等环境特征及物理量场特征。结果表明:这次暴雨过程粤西地区共经历两次强降水过程,分别是受飑线系统、以及高空槽和低空切变影响;西南低空急流的出现有利于粤西暴雨的形成、维持和发展;暴雨过程粤西上空垂直累积液水含量达25~30g/m2;暴雨期间风向随高度明显逆转,有冷平流输送;约2.0 km高度以下低空急流的下传和增强与暴雨的产生有密切关系;短时间内多普勒天气雷达的速度回波低层辐合区域远远大于辐散区域是可能产生强降水的标志。     

南昌地铁二号线隧道开挖风险性可拓学评价

地铁建设中始终面临着隧道开挖风险和毗邻建筑环境的风险,对其进行详细评价并找出主要影响风险源,对于控制工程风险、提高工程安全性和投资效益是地铁工程建设不可忽视的重要环节。应用可拓学方法,分别对南昌地铁二号线翠苑路-地铁大厦区间的隧道开挖风险和毗邻开挖区的建筑环境的风险进行评价,找出了最主要的风险影响因子,对同类工程建设具有借鉴意义。     

2000—2020年中国人口分布格局演变及影响因素

基于第五、六、七次全国人口普查数据,本文分析了2000—2020年中国人口分布的空间格局、集散态势和影响因素。结果表明,中国人口分布依然保持东密西疏的基本格局,胡焕庸线两侧的自然地理环境差异性决定了这一格局的长期稳定性;人口空间集中化趋势在21世纪初的10年内主要发生在东南半壁,但在2010—2020年间成为各区域的共同特征。省会城市的人口集聚能力持续增强,2010—2020年的优势更加凸显,但这种行政力量主导的首位度提升效应将随着全省发展阶段的演进而逐渐弱化。人口变动的区域分化明显：沿海城市群的空间连绵化逐渐形成了强吸引力、高承载力的沿海人口增长带,东北地区几乎转向全面的人口收缩,中部各省依托省会展开的人口竞争依然激烈,川渝黔地区普遍实现了人口的止降回增,西北地区则面临人口收缩风险。此外,区域人口增长的驱动因素逐渐从经济要素主导转为经济要素和舒适性要素并重,各地区舒适性的差异可能将成为影响未来人口空间格局变化的重要因素。     

基于网络文本的廊道型旅游地意象研究——以皖南“川藏线”为例

旅游地意象是旅游地理学的重要研究主题,旅游者具身化意象认知结果对旅游地行为忠诚、满意度及旅游资源开发至关重要。借助蕴含旅游者记忆与叙事信息的网络游记文本及图片位置数据,采用质性与GIS分析相结合的方法,建构廊道型旅游地意象。研究发现：1）廊道型旅游地意象由线性意象、色彩意象、地方意象、审美意象和情感意象五维类属建构而成。2）皖南“川藏线”旅游者在场体验过程中的情感评价积极情感占主导地位,消极情感占比相对较少,其中高度积极情感所占比例显著高于高度消极情感。3）旅游者皖南“川藏线”意象要素感知特征呈现动静结合、线性体验与感知兼具两个层级。其中,动静特征通过静态景观与动态体验共同展现,线性体验更多强调旅游者产生的刺激、惊险、震撼的驾驶乐趣及情感升华。4）皖南“川藏线”线性意象热点集中于桃岭公路及六道湾周边,色彩意象热点集中于储家滩和红杉林两地,审美意象热点集中于储家滩、青龙湖、红杉林沿线,地方意象热点集中于储家滩、桃岭公路和水墨汀溪一带。     

星系NGC5018的星族合成研究

利用星团谱样本的星族合成方法,研究了邻近巨椭圆星系NGC5018中的星族成分和其内部的恒星形成历史,给出了星系中不同年龄和金属丰度星族的成分占有比.星族合成结果表明,NGC5018中不仅存在大量金属丰度低的年老恒星成分,而且较年轻的星族成分(T=5×108yr)对星系光度贡献也很重要.星系吞并和相互作用过程可能是触发这些较年轻星族形成的物理原因,椭圆星系内部的恒星形成历史可能是2次爆发或者多次爆发过程.这些结果可以很好地解释NGC5018颜色偏蓝、Mg2谱指数强度偏弱等观测特征.     

Ion contribution to the astrophysical important 388.86, 471.32 and 501.56 nm He I spectral lines broadening

Characteristics of the astrophysical important Stark broadened 388.86 nm, 471.32 nm and 501.56 nm He I spectral line profiles have been measured at electron densities between 4.4·10²² and 8.2·10²² m⁻³ and electron temperatures between 18,000 and 33,000 K in plasmas created in five various discharge conditions using a linear, low-pressure, pulsed arc as an optically thin and reproductive plasma source operated in a helium–nitrogen–oxygen gas mixture. On the basis of the observed asymmetry of the line profiles, we have obtained their ion broadening parameters (A) caused by influence of the ion microfield and also the influence of the ion dynamic effect (D) to the line shape. Our A and D parameters represent the first data obtained experimentally by the use of the line profile deconvolution procedure. We have found stronger influence of the ion contribution to these He I line profiles than the semiclassical theoretical approximation provides. This can be important for some astrophysical plasma modelling or for diagnostics.     

Partial redistribution effects on line polarization in the presence of velocity fields

Velocity fields in line formation regions strongly affect the line polarization. The conventionally used observer's frame method of solving the polarized transfer equation becomes expensive and inaccurate for partial redistribution problems, when large amplitude velocity fields have to be considered in the observer's frame. An alternative method of solution is the comoving frame method. Partial redistribution problems are solved using comoving frame formalism for line polarization caused by resonance scattering.     

Paleo-glacial reconstruction of the Thajwas glacier in the Kashmir Himalaya using 10Be cosmogenic radionuclide dating

Quantitative glacial chronologies of past glaciations are sparse in the Himalaya, and mostly absent in the Kashmir Himalaya. We used cosmogenic ¹⁰Be exposure dating, and geomorphological mapping to reconstruct glacial advances of the Thajwas Glacier (TG) in the Great Himalayan Range of the Kashmir Himalaya. From ¹⁰Be exposure dating of ten moraine boulders, four glacial stages with ages ～20.77 ± 2.28 ka, ～11.46 ± 1.69 ka, ～9.12 ± 1.39 ka and ～4.19 ± 0.78 ka, were identified. The reconstructed cosmogenic radionuclide ages confirmed the global Last Glacial Maximum (gLGM), Younger Dryas, Early Holocene, and Neoglaciation episodes. As per area and volume change analyses, the TG has lost 51.1 km² of its area and a volume of 2.64 km³ during the last 20.77 ± 2.28 ka. Overall, the results suggested that the TG has lost 64% of area and 73% of volume from the Last glacial maximum to Neoglaciation and about 85.74% and 87.67% of area and volume, respectively, from Neoglaciation to the present day. The equilibrium line altitude of the TG fluctuated from 4238 m a.s.l present to 3365 m a.s.l during the gLGM (20.77 ± 2.28 ka). The significant cooling induced by a drop in mean ambient temperature resulted in a positive mass balance of the TG during the gLGM. Subsequently the melting accelerated due to the continuing rise of the global ambient temperature. Paleo-glacial history reconstruction of the Kashmir Himalaya, with its specific geomorphic and climatic setting, would help close the information gap about the chronology of past regional glacial episodes.     

飑线的研究进展

飑线是一种线状的中尺度对流系统,发生时破坏力大,可以产生严重的经济损失和人员伤亡。在我国,几乎每年都会出现由飑线引起的巨大损失。近年来,国内外对飑线的研究不断发展,无论是从大尺度环流背景、形成机制、组织形式、内部结构还是维持机制都有了较为深入的研究。深入研究飑线的形成过程,对于预报和灾害预警、防护,都具有很重要的意义。     

The iron Kα lines as a tool for magnetic field estimations in non-flat accretion flows

Observations of AGNs and microquasars by ASCA, RXTE, Chandra and XMM-Newton indicate the existence of broad X-ray emission lines of ionized heavy elements in their spectra. Such spectral lines were discovered also in X-ray spectra of neutron stars and X-ray afterglows of GRBs. Recently, Zakharov et al. [MNRAS 342 (2003) 1325] described a procedure to estimate an upper limit of the magnetic fields in regions from which X-ray photons are emitted. The authors simulated typical profiles of the iron Kα line in the presence of magnetic field and compared them with observational data in the framework of the widely accepted accretion disk model. Here we further consider typical Zeeman splitting in the framework of a model of non-flat accretion flows, which is a generalization of previous consideration into non-equatorial plane motion of particles emitting X-ray photons. Using perspective facilities of space borne instruments (e.g., Constellation-X mission) a better resolution of the blue peak structure of iron Kα line will allow to evaluate the magnetic fields with higher accuracy.